  In this Letter, the broad emission line (BEL) profiles of superluminal
quasars with apparent jet velocities, $\beta_{a}>10$, (ultraluminal QSOs, or
ULQSOs hereafter) are studied as a diagnostic of the velocity field of the BEL
emitting gas in quasars. The ULQSOs are useful because they satisfy a very
strict kinematical constraint, their parsec scale jets must be propagating
within $12^{\circ}$ of the line of sight. We know the orientation of these
objects with great certainty. The large BEL FWHM, $\sim 3,000 \mathrm{km/s} -
6,000 \mathrm{km/s}$, in ULQSOs tend to indicate that the BEL gas has a larger
component of axial velocity (either random or in a wind) along the jet
direction than previously thought.
