QSO Host Galaxy Luminosity and [OIII] Line Width as a Surrogate for Stellar Velocity Distribution

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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.