What does Civ{\lambda}1549 tell us about the physical driver of the
  Eigenvector Quasar Sequence?
  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.
