  We present a systematic study of ionized gas outflows based on the velocity
shift and dispersion of the [O III] {\lambda}5007 $\AA$ emission line, using a
sample of ~ 5000 Type 1 AGNs at z < 0.3 selected from Sloan Digital Sky Survey.
This analysis is supplemented by the gas kinematics of Type 2 AGNs from Woo et
al. (2016). For the majority of Type 1 AGNs (i.e., ~ 89%), the [O III] line
profile is best represented by a double Gaussian model, presenting the
kinematic signature of the non-virial motion. Blueshifted [O III] is more
frequently detected than redshifted [O III] by a factor of 3.6 in Type 1 AGNs,
while the ratio between blueshifted to redshifted [O III] is only 1.08 in Type
2 AGNs due to the projection and orientation effect. The fraction of AGNs with
outflow signatures is found to increase steeply with [O III] luminosity and
Eddington ratio, while Type 1 AGNs have larger velocity dispersion and more
negative velocity shift than Type 2 AGNs. The [O III] velocity - velocity
dispersion (VVD) diagram of Type 1 AGNs expands towards higher values with
increasing luminosity and Eddington ratio, suggesting that the radiation
pressure or wind is the main driver of gas outflows, as similarly found in Type
2 AGNs. In contrast, the kinematics of gas outflows is not directly linked to
the radio activity of AGN.
