The Line Emission Region in III Zw 2: Kinematics and Variability

Abstract

We have studied the Ly-al, Hbeta, Halpha and Mg II2798 line profiles of the Seyfert 1 galaxy III Zw 2. The shapes of these broad emission lines show evidence of a multicomponent origin and also features which may be identified as the peaks due to a rotating disk. We have proposed a two-component Broad Line Region (BLR) model consisting of an inner Keplerian relativistic disk and an outer structure surrounding the disk. The results of the fitting of the four Broad Emission Lines (BELs) here considered, are highly consistent in both the inner and outer component parameters. Adopting a mass of approx. 2 E8 sollar masses for the central object we found that the outer radius of the disk is approximately equal for the four considered lines (approx 0.01 pc). However, the inner radius of the disk is not the same: 0.0018 pc for Ly-alpha, 0.0027 pc for Mg II, and 0.0038 pc for the Balmer lines. This as well as the relatively broad component present in the blue wings of the narrow [OIII] lines indicate stratification in the emission-line region. Using long-term Hbeta observations (1972-1990, 1998) we found a flux variation of the BEL with respect to the [OIII] lines.Comment: ApJ, accepted, 22 pages, 10 figure

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

“…The other 8% of objects, with uncertain continuum determination, do not affect the final result. Popović et al 2003). It has been assumed that all UV Fe II lines in this range are originating in the same emission region and consequently to have the same Doppler width and shift.…”

Balmer lines emission region in NGC 3516: Kinematical and physical properties

“…To limit the number of free parameters in the fit of the Hβ line we have also set some a priori restrictions on the narrow components and satellite lines (Popović & Mediavilla 1997;Popović et al 2001Popović et al , 2002. In the first place, the three narrow Gaussians representing the two [OIII]λλ4959, 5007 lines and the narrow Hβ component are preconditioned to have the same redshift and full widths proportional to their wavelengths.…”

“…One possibility is that the central dip of the line associated to the disk geometry may be masked by broad emission coming from elsewhere. A two component model including an accretion disk and a region with different geometry covering the disk has satisfactorily described the emission lines of Akn 120 (Popović et al 2001) and III Zw 2 (Popović et al 2002).…”

“…van Groningen 1987;Sulentic et al 1998;Sulentic 1999;Popović et al 2001Popović et al , 2002. One possibility is that the central dip of the line associated to the disk geometry may be masked by broad emission coming from elsewhere.…”

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

“…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.…”