  Broad emission lines in quasars enable us to "resolve" structure and
kinematics of the broad line emitting region (BLR) thought to in- volve an
accretion disk feeding a supermassive black hole. Interpretation of broad line
measures within the 4DE1 formalism simplifies the apparent confusion among such
data by contrasting and unifying properties of so-called high and low accreting
Population A and B sources. H{\beta} serves as an estimator of black hole mass,
Eddington ratio and source rest frame, the latter a valuable input for
Civ{\lambda}1549 studies which allow us to isolate the blueshifted wind
component. Optical and HST-UV spectra yield H{\beta} and Civ{\lambda}1549
spectra for low-luminosity sources while VLT-ISAAC and FORS and TNG-LRS provide
spectra for high Luminosity sources. New high S/N data for Civ in
high-luminosity quasars are presented here for comparison with the other
previously published data. Comparison of H{\beta} and Civ{\lambda}1549 profile
widths/shifts indicates that much of the emission from the two lines arise in
regions with different structure and kinematics. Covering a wide range of
luminosity and redshift shows evidence for a correlation between
Civ{\lambda}1549 blueshift and source Eddington ratio, with a weaker trend with
source luminosity (similar amplitude outflows are seen over 4 of the 5 dex
luminosity range in our combined samples). At low luminosity (z < 0.7) only
Population A sources show evidence for a significant outflow while at high
luminosity the outflow signature begins to appear in Population B quasars as
well.
