[O iii] 5007 Å Emission Line Width as a Surrogate for σ _∗ in Type 1 AGNs?

We present a study of the relation between [OIII] 5007A emission line width (sigma_{[OIII]}) and stellar velocity dispersion (sigma_{*}), utilizing sample 740 type 1 active galactic nuclei (AGNs) with high-quality spectra at redshift z < 1.0. find broad correlation core component (sigma_{[OIII,core]}) sigma_{*} scatter 0.11~dex for low (z 0.1) sample; (0.3 1.0) AGNs, is larger, being 0.16~dex. also that Eddington ratio (L_{bol}/L_{Edd}) may play an important role in discrepancies sigma_{[OIII,core]} sigma_{*}. As L_{bol}/L_{Edd} increases, tends to be larger than By classifying our local different minor-to-major axis ratios, we those edge-on spiral galaxies. In addition, effects outflow strength properties such as maximum (V_{max}) broader shift (sigma_{[OIII,out]} V_{[OIII,out]}) major The are when V_{max}, V_{[OIII,out]}, sigma_{[OIII,out]} increase. Our results show strengths have significant on differences narrow-line region gas kinematics AGNs. suggest caution should taken using surrogate substitute could used only luminosity