  Supermassive black holes in galactic nuclei show a close relationship between
the black hole mass, luminosity, and stellar velocity dispersion (sigma_*) of
the host galaxy bulge. Probing these relationships at high redshift may shed
light on the link between the formation of the galactic bulge and central black
hole, but direct measurements of stellar velocity dispersion at high redshift
are difficult. We show that [OIII] line widths provide a useful surrogate for
sigma_* by comparing sigma_[OIII] with the value of sigma_* predicted by the
Faber-Jackson relation for QSOs with measured host galaxy luminosity. Over a
wide range of AGN luminosity, sigma_[OIII] tracks sigma_*, albeit with
considerable scatter. [OIII] line widths are narrower by ~0.1 dex in radio-loud
QSOs than in radio-quiet QSOs of similar host luminosity. In low redshift QSOs,
the ratio of star formation rate to black hole growth rate is much smaller than
the typical ratio of bulge mass to black hole mass.
