Contribution of the disk emission to the broad emission lines in AGNs: Two-component model

Free access article

Issue		A&A Volume 423, Number 3, September I 2004


Page(s)		909 - 918
Section		Extragalactic astronomy
DOI		http://dx.doi.org/10.1051/0004-6361:20034431

A&A 423, 909-918 (2004)
DOI: 10.1051/0004-6361:20034431

Contribution of the disk emission to the broad emission lines in AGNs: Two-component model

L. C. Popovic^{1, 2, 3}, E. Mediavilla⁴, E. Bon^{1, 3} and D. Ilic⁵

¹ Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia
    e-mail: [lpopovic;ebon]@aob.bg.ac.yu
² Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany (Alexander von Humboldt fellow)
    e-mail: lpopovic@aip.de
³ Isaac Newton Institute of Chile, Yugoslavia Branch, Yugoslavia
⁴ Instituto de Astrofísica de Canarias C/ Vía Làctea, s/n 38200 La Laguna, Tenerife, Spain
    e-mail: emg@ll.iac.es
⁵ Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, 11000 Belgrade, Serbia
    e-mail: dilic@matf.bg.ac.yu

(Received 2 October 2003 / Accepted 3 May 2004)

Abstract
We present an investigation of the structure of the emission line region in a sample of 12 single-peaked Active Galactic Nuclei (AGNs). Using the high resolution H $\beta$ and H $\alpha$ line profiles observed with the Isaac Newton Telescope (La Palma) we study the substructure in the lines (such as shoulders or bumps) which can indicate a disk or disk-like emission in Broad Line Regions (BLRs). Applying Gaussian analysis we found that both kinds of emission regions, BLR and NLR, are complex. In this sample the narrow [OIII] lines are composites of two components; NLR1 which have random velocities from ~200 to 500 km s ^-1 and systematic velocities toward the blue from 20 to 350 km s ^-1, and NLR2 with smaller random velocities (~100-200 km s ^-1) and a redshift corresponding to the cosmological one. The BLR also have complex structure and we apply a two-component model assuming that the line wings originate in a very broad line region (VBLR) and the line core in an intermediate line region (ILR). The VBLR is assumed to be an accretion disk and the ILR a spherical emission region. The model fits very well the H $\alpha$ and H $\beta$ line profiles of the AGNs.

Key words: galaxies: Seyfert -- line: profiles -- accretion, accretion disks

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