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Using a sample of 24264 optically selected AGNs from the SDSS DR7 database,we characterise how the profile of the [OIII] emission line relates tobolometric luminosity (L_Bol), Eddington ratio, radio loudness, radioluminosity (L_Rad) and optical class (Sy 1/2) to determine what drives thekinematics of this kpc-scale line emitting gas. Spectral stacking is used tocharacterise how the average [OIII] profile changes as a function of thesevariables. After accounting for the correlation between L_Bol and L_Rad, wereport that L_Rad has the strongest influence on the [OIII] profile, withmoderate radio luminosity AGNs (log(L_Rad)=23-25 W/Hz) having the broadest[OIII] profiles. When binned according to Eddington ratio, only AGNs in ourhighest bin (i.e., R_Edd>0.3) show any signs of having broadened [OIII]profiles, although the small numbers of such extreme AGNs mean we cannot ruleout that other processes (e.g., radio jets) are responsible for thisbroadening. We find no significant difference between the [OIII] profiles ofbroad and narrow-line Seyfert 1s. The [OIII] profiles of Sy 1 and 2 AGNs showthe same trends in terms of line width, but Sy 1 AGNs display a much strongerblue wing, which we interpret as evidence of outflowing ionised gas. Usingmulti-component line fitting we calculate the proportions of AGNs with broad[OIII] profiles, finding that moderate radio luminosity AGNs are roughly 5times more likely to have extremely broad [OIII] lines (FWHM>1000km/s) comparedto lower L_Rad AGNs. Our results are consistent with the most disturbed gaskinematics being induced by compact radio cores (rather than powerful radiojets), although broadened [OIII] lines are also present, but much rarer, in lowL_Rad systems (<10^23 W/Hz). Our catalogue of multi-component fits is freelyavailable as an online resource.

Narrow-line region gas kinematics of 24,264 optically-selected AGN: the radio connection