  To investigate AGN outflows as a tracer of AGN feedback on star-formation, we
perform integral-field spectroscopy of 20 type 2 AGNs at z<0.1, which are
luminous AGNs with the [O III] luminosity >10$^{41.5}$ erg/s, and exhibit
strong outflow signatures in the [O III] kinematics. By decomposing the
emission-line profile, we obtain the maps of the narrow and broad components of
[O III] and H$\alpha$ lines, respectively. The broad components in both [O III]
and H$\alpha$ represent the non-gravitational kinematics, i.e., gas outflows,
while the narrow components, especially in H$\alpha$, represent the
gravitational kinematics, i.e., rotational disk. By using the integrated
spectra within the flux-weighted size of the narrow-line region, we estimate
the energetics of the gas outflows. The ionized gas mass is 1.0-38.5$\times
10^5$ $M_{\odot}$, and the mean mass outflow rate is 4.6$\pm$4.3
$M_{\odot}$/yr, which is a factor of ~260 higher than the mean mass accretion
rate 0.02$\pm$0.01 $M_{\odot}$/yr. The mean energy injection rate of the sample
is 0.8$\pm$0.6% of the AGN bolometric luminosity, while the momentum flux is
(5.4$\pm$3.6)$\times$ $L_{bol}$/c on average, except for two most kinematically
energetic AGNs with low $L_{bol}$, which are possibly due to the dynamical
timescale of the outflows. The estimated outflow energetics are consistent with
the theoretical expectations for energy-conserving outflows from AGNs, yet we
find no supporting evidence of instantaneous quenching of star formation due to
the outflows.
