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Long-term profile variability of double-peaked emission lines in AGNs

Published online by Cambridge University Press:  24 November 2004

K. T. Lewis
Affiliation:
Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA
M. Eracleous
Affiliation:
Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA
J. P. Halpern
Affiliation:
Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA
T. Storchi-Bergmann
Affiliation:
Instituto de Fisica, UFRGS, 91501-970 Porto Alegre, RS, Brazil
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Abstract

An increasing number of AGNs exhibit broad, double-peaked Balmer emission lines, which arise from the outer regions of the accretion disk which fuels the AGN. The line profiles vary on timescales of 5–10 years. Our group has monitored a set of 20 double-peaked emitters for the past 8 years (longer for some objects). Here we describe a project to characterize the variability patterns of the double-peaked Hα line profiles and compare with those of two simple models: a circular disk with a spiral arm and an elliptical disk.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

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Copyright
© 2004 International Astronomical Union
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Long-term profile variability of double-peaked emission lines in AGNs
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