THE CONNECTIONS BETWEEN THE UV AND OPTICAL Fe ii EMISSION LINES IN TYPE 1 AGNs

Abstract

We investigate the spectral properties of the UV (λλ2650-3050Å) and optical (λλ4000-5500Å) Fe II emission features in a sample of 293 type 1 active galactic nuclei (AGNs) from Sloan Digital Sky Survey (SDSS) database. We

Virilization of the Broad Line Region in Active Galactic Nuclei—connection between shifts and widths of broad emission lines

“…We choose the sample with the broad Hβ and Mg II λ2800Å lines (their equivalent widths requested to be larger than zero) in the redshift range 0.407 ≤ z ≤ 0.643. This sample of 293 AGN is initially used for research of the relations between the UV and optical Fe II emission in the Type 1 AGN, so the detailed search criteria and fitting procedures are given in Kovačević-Dojčinović & Popović (2015). After eliminating the spectra with very noisy UV part, near the Mg II line, our sample contained 287 AGN spectra.…”

“…Bon et al 2009a;Kovačević et al 2010), which supports the twocomponent model of the BLR (Popović et al 2004;Bon et al 2006;Hu et al 2008). The detailed description of this multi-Gaussian model and the fitting procedure is given in Kovačević-Dojčinović & Popović (2015), where fitting of this sample is performed in two spectral ranges: UV (2650-3050) and optical (4000-5500).…”

“…After that, we fit simultaneously the UV Fe II lines in the range 2650-3050Å with the Mg II line. For the UV Fe II lines we use the model described in Popović et al (2003) and Kovačević-Dojčinović & Popović (2015). Note that the Mg II line is the resonant doublet Mg IIλλ 2795, 2803 A.…”

Black Hole Mass Estimation in Type 1 AGN: Hβ vs. Mg II Lines and the Role of Balmer Continuum

“…The Mg II line was fitted with two Gaussian functions, the one that represents the line core and the other that fits the line wings (see Kovačević-Dojčinović and Popović, 2015), and a sum of those two components represents the broad Mg II line. The narrow Mg II line was not detected in analyzed spectra.…”

“…The narrow Mg II line was not detected in analyzed spectra. The numerous Fe II lines in the range 2,650-3,050Å were all fitted with the Fe II template presented in Popović et al (2003) and Kovačević-Dojčinović and Popović (2015). The Fe II lines in the 2,650-3,050Å range were divided into four multiplets, and relative intensities of the lines within each multiplet were taken from literature.…”