A comparison of stellar and gaseous kinematics in the nuclei of active galaxies

To investigate the relationship between black holes and their host galaxies, many groups have used the width of the [O III] λ5007 line as a substitute for the stellar velocity dispersion (σ*) of galaxy bulges. We directly test this assumption with a large and homogeneous sample of narrow-line active galactic nuclei from the Sloan Digital Sky Survey. We consider multiple transitions ([O II] λ3727, [O III] λ5007, and [S II] λλ6716, 6731) and various techniques for quantifying the line width in order to obtain a calibration between the gas velocity dispersion, σ_g, and σ*. We find that σ_g of the low-ionization lines traces σ*, as does σ_g for the core of [O III] after its asymmetric blue wing is properly removed, although in all cases the correlation between σ_g and σ* has considerable scatter. While the gas kinematics of the narrow-line region of active galaxies are primarily governed by the gravitational potential of the stars, the accretion rate, as traced by the Eddington luminosity ratio, seems to play an important secondary role. Departures from virial motions correlate systematically with accretion rate. We discuss the implications of these results for previous studies that use [O III] line widths to infer stellar velocity dispersions in quasars and narrow-line Seyfert 1 galaxies.