  We present gas kinematics based on the [OIII] $\lambda$5007 line and their
connection to galaxy gravitational potential, active galactic nucleus (AGN)
energetics, and star formation, using a large sample of ~110,000 AGNs and
star-forming (SF) galaxies at z<0.3. Gas and stellar velocity dispersions are
comparable to each other in SF galaxies, indicating that the ionized gas
kinematics can be accounted by the gravitational potential of host galaxies. In
contrast, AGNs clearly show non-gravitational kinematics, which is comparable
to or stronger than the virial motion caused by the gravitational potential.
The [OIII] velocity-velocity dispersion (VVD) diagram dramatically expands
toward high values as a function of AGN luminosity, implying that the outflows
are AGN-driven, while SF galaxies do not show such a trend. We find that the
fraction of AGNs with a signature of outflow kinematics, steeply increases with
AGN luminosity and Eddington ratio. In particular, the majority of luminous
AGNs presents strong non-gravitational kinematics in the [OIII] profile. AGNs
with strong outflow signatures show on average similar specific star formation
rate (SSFR) to that of starforming galaxies. In contrast, AGNs with weak or no
outflows have an order of magnitude lower SSFR, suggesting that AGNs with
current strong outflows do now show any negative AGN feedback and that it may
take the order of a dynamical time to impact on star formation over galactic
scales.
