  We explore the relationship between the ionized gas outflows and radio
activity using a sample of $\sim$ 6000 AGNs at z < 0.4 with the kinematical
measurement based on the [O III] line profile and the radio detection in the
VLA FIRST Survey. To quantify radio activity, we divide our sample into a
series of binary subclasses based on the radio properties, i.e.,
radio-luminous/radio-weak, AGN-dominated/star-formation-contaminated,
compact/extended, and radio-loud/radio-quiet. None of the binary subclasses
exhibits a significant difference in the normalized [O III] velocity dispersion
at a given [O III] luminosity once we correct for the influence of the host
galaxy gravitational potential. We only detect a significant difference of [O
III] kinematics between high and low radio-Eddington ratio (L$_{1.4
GHz}$/L$_{Edd}$) AGNs. In contrast, we find a remarkable difference in ionized
gas kinematics between high and low bolometric-Eddington ratio AGNs. These
results suggest that accretion rate is the primary mechanism in driving ionized
gas outflows, while radio activity may play a secondary role providing
additional influence on gas kinematics
