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Broad emission lines in quasars enable us to "resolve" structure andkinematics of the broad line emitting region (BLR) thought to in- volve anaccretion disk feeding a supermassive black hole. Interpretation of broad linemeasures within the 4DE1 formalism simplifies the apparent confusion among suchdata by contrasting and unifying properties of so-called high and low accretingPopulation 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 forCiv{\lambda}1549 studies which allow us to isolate the blueshifted windcomponent. Optical and HST-UV spectra yield H{\beta} and Civ{\lambda}1549spectra for low-luminosity sources while VLT-ISAAC and FORS and TNG-LRS providespectra for high Luminosity sources. New high S/N data for Civ inhigh-luminosity quasars are presented here for comparison with the otherpreviously published data. Comparison of H{\beta} and Civ{\lambda}1549 profilewidths/shifts indicates that much of the emission from the two lines arise inregions with different structure and kinematics. Covering a wide range ofluminosity and redshift shows evidence for a correlation betweenCiv{\lambda}1549 blueshift and source Eddington ratio, with a weaker trend withsource luminosity (similar amplitude outflows are seen over 4 of the 5 dexluminosity range in our combined samples). At low luminosity (z < 0.7) onlyPopulation A sources show evidence for a significant outflow while at highluminosity the outflow signature begins to appear in Population B quasars aswell.

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