SIMBAD references

Galaxy bulge luminosity L, black hole mass M_BH, and stellar velocity dispersion σ_*increase together in a way suggesting a close evolutionary relationship. Measurements of the M_BH-σ_*relationship as a function of cosmic time may shed light on the origin of this relationship. Direct measurements of σ_*at high redshift are difficult, and the width of the narrow emission lines of active galactic nuclei (AGN) has been proposed as a surrogate for σ_*. We investigate the utility of using σ_[OIII]_for σ_*by examining host galaxy magnitudes and [O III] line widths for low-redshift QSOs. For radio-quiet QSOs, σ_[OIII]_is consistent in the mean with the value of σ_*predicted by the Faber-Jackson relation. For our limited range of L_host, scatter obscures the expected increase of σ_[OIII]_with L_host. However, for a sample of AGN covering a wide range of measured or inferred σ_*, there is a clear increase of σ_[OIII]_with σ_*. Radio-loud QSOs on average have σ_[OIII]_smaller by 0.1 dex than radio-quiet QSOs of similar L_host, at least for luminosities typical of PG QSOs. Star formation rates in our low-redshift QSOs are smaller than required in order to maintain the typical observed ratio of bulge mass to black hole mass.