Xue–Guang Zhang,1,2 Deborah Dultzin–Hacyan,1 and Ting–Gui Wang2
1 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70–264, México D. F. 04510, México (deborah@astroscu.unam.mx, xguang@astroscu.unam.mx)
2 Center for Astrophysics, Department of Astronomy and Applied Physics, University of Science and Technology of China, Hefei, Anhui, P.R. China (twang@ustc.edu.cn)
Received 2006 May 24
Accepted 2006 October 17
]]> RESUMEN
Estudiamos las propiedades de una muestra de 27 núcleos activos de galaxias (NAGs) con perfil de doble pico (dbp) en las líneas anchas de emisión de baja ionización, tomados del DR4. Nuestro primer resultado es que todo el espectro de emisión en el intervalo de 4100 Å a 5800 Å se puede ajustar muy bien mediante un modelo de emisión en un disco de acreción elíptico. Los mejores ajustes indican que la emisión óptica de las líneas de FeII en los emisores dbp se originan en la misma región del disco que las líneas de Balmer. Encontramos que algunas correlaciones conocidas para los NAGs normales se cumplen también para los dbp. Sin embargo, este resultado debe tomarse con cautela porque el número de objetos es pequeno y porque tenemos un sesgo de selección hacia objetos con emisión de FeII intensa. Mostramos que para los dbp, la masa del agujero negro central parece tener mayor influencia en las propiedades de la emisión de FeII que la tasa de acreción.
ABSTRACT
We study the FeII properties of double–peaked broad low–ionization emission line AGN (dbp emitters) using a sample of 27 dbp emitters from SDSS (DR4). Our first result is that the line spectra in the wavelength range from 4100 Å to 5800 Å can be best fitted by an elliptical accretion disk model.The best fitted results indicate that the optical FeII emission lines of dbp emitters originate from the same region in the accretion disk where the double–peaked Balmer emission lines originate. Some correlations between FeII emission lines and the other broad emission lines for normal AGN can be confirmed for dbp emitters. However, these results should be taken with caution due to the small number of objects and the bias in selecting strong FeII emitters. We show that for dbp emitters, BH masses seems to have more influence on FeII properties than dimensionless accretion rate.
Key Words: ACCRETION, ACCRETION DISKS — GALAXIES: ACTIVE — QUASARS: EMISSION LINES
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ACKNOWLEDGEMENTS
]]> ZXG gratefully acknowledges the postdoctoral scholarships offered by Universidad Nacional Autónoma de México (UNAM). D. D–H acknowledges support from grant IN100703 from DGAPA, UNAM. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This paper has also made use of the data from the SDSS projects. Funding for the creation and the distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbuka–gakusho, and the Max Planck Society. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, Institute for Advanced Study, Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, Max–Planck–Institute for Astronomy (MPIA), Max–Planck–Institute for Astrophysics (MPA), New Mexico State University, Princeton University, United States Naval Observatory, and University of Washington.
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