We present a spectroscopic study of broad lines in the UV for a sample of 42 type 1 high accreting quasars at z = 2.2 from SDSS-DR12. The basis of this work are multi-component fits made with the IRAF specfit routine in three regions of the spectra centered at 1900, 1550 and 1400 A where the main emissions of C III, C IV and Si IV + O IV] are found respectively.
By comparing flux ratios of UV emision lines (i.e. Al III / C IV, Si IV / He II) as metallicity indicators with Cloudy photoionization models we were able to attribute a ionization parameter log(U) = 0 to the non virialized gas in the BLR and derive the metal content of our sample within the range 5 < Z < 20 Z\odot, this suggests that the accretion rate is related to the enrichment of the host galaxy. We also derived physical parameters and reach out for correlations between them and flux ratios finding out that the ratio C III / Si III behaves as a viral estimator.
Enviado por garlaaaa@hotmail.com, 2019 Oct