  QSOs' emission lines arise from highest velocity (approximately 10000 km/s),
dense gas within approximately 0.1 parsec of the central engine, out to
low-velocity, low-density gas at great distances from the host galaxy. In
radio-loud QSOs there are clear indications that the distribution and
kinematics of emission-line gas are related to the symmetry axis of the central
engine, as defined by the radio jet. These jets originate at nuclear distances
< 0.1 pc --- similar to the highest-velocity emission line gas. There are two
ways we can investigate the different environments of radio-loud and
radio-quiet QSOs, i.e., those with and without powerful radio jets. One is to
look for optical-UV spectroscopic differences between radio-loud and
radio-quiet QSOs. The other is to investigate dependences of spectroscopic
properties on properties of the powerful jets in radio-loud QSOs. Here we
summarize the spectroscopic differences between the two classes, and present
known dependences of spectra on radio core-dominance, which we interpret as
dependences on the angle of the central engine to the line-of-sight. We
speculate on what some of the differences may mean.
