http://arxiv.org/abs/1509.03679
We investigate the spectral properties of the UV (2650-3050 A) and optical (4000-5500 A) FeII emission features in a sample of 293 type 1 AGNs from SDSS database. We explore different correlations between their emission line properties, as well as the correlations with the other emission lines from the spectral range. We find several interesting correlations and we can outline the most interesting results as: (i) there is a kinematical connection between the UV and optical FeII lines indicating that the UV and optical FeII lines originate from the outer part of the Broad Line Region, so-called Intermediate Line Region (ILR); (ii) the unexplained anticorrelations of the optical FeII (EW FeII_opt vs. EW [OIII]5007A and EW FeII_opt vs. FWHM Hbeta) have not been detected for the UV FeII lines; (iii) the significant averaged redshift in the UV FeII lines, that is not present in optical FeII, indicates an inflow in the UV FeII emitting clouds and probably their asymmetric distribution; (iv) we confirm the anticorrelation between the intensity ratio of optical and UV FeII lines vs. FWHM of Hbeta, and we find the anticorrelations of this ratio with the widths of MgII 2800 A, optical FeII and UV FeII. This indicate a very important role of the column density and microturbulence in the emitting gas. We discuss the starburst activity in high density regions of young AGNs, as a possible explanation of the detected optical FeII correlations and intensity line ratios of the UV and optical FeII lines.
J. Dojcinovic and L. Popovic
Tue, 15 Sep 15
78/83
Comments: 62 pages, 19 figures, accepted in ApJS
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