  It has been previously determined that there is a highly significant
correlation between the spectral index from 10 GHz to 1350 $\AA$ and the amount
of excess luminosity in the red wing of quasar CIV $\lambda$1549 broad emission
lines (BELs). Ostensibly, the prominence of the red excess is associated with
the radio jet emission mechanism and is most pronounced for lines of sight
close to the jet axis. Studying the scant significant differences in the UV
spectra of radio loud and radio quiet quasars might provide vital clues to the
origin of the unknown process that creates powerful relativistic jets that
appear in only about ten percent of quasars. In this study, the phenomenon is
explored with multi-epoch observations of the MgII $\lambda$2798 broad line in
3C 279 which has one of the largest known redwing excesses in a quasar
spectrum. The amount of excess that is detected appears to be independent of
all directly observed optical continuum, radio or submm properties (fluxes or
polarizations). The only trend that occurs in this sparse data is: the stronger
the BEL, the larger the fraction of flux that resides in the redwing. It is
concluded that more monitoring is needed and spectropolarimetry with a large
telescope is essential during low states to understand more.
