  There is an ongoing debate on whether feedback from active galactic nuclei
(AGNs) can effectively regulate the star formation activities in their host
galaxies. To investigate the feedback effect of AGN-driven outflows, we perform
integral-field spectroscopic observations of 40 moderate-luminosity
(10$^{41.5}$ $<$ L$_{\rm [OIII];cor}$ $<$ 10$^{43.1}$ erg s$^{-1}$) Type-2 AGNs
at z $<$ 0.1, which present strong outflow signatures in the integrated [OIII]
kinematics. Based on the radial profile of the normalized [OIII] velocity
dispersion by stellar velocity dispersion, we measure the kinematic outflow
size and extend the kinematic outflow size-luminosity relation reported in Kang
& Woo (2018) into a wider luminosity range (over four orders of magnitude in
[OIII] luminosity). The shallow slope of the kinematic outflow size-luminosity
relation indicates that while ionizing photons can reach out further, kinetic
energy transfer is much less efficient due to various effects, demonstrating
the importance of kinematical analysis in quantifying the outflow size and
energetics. By comparing the outflow kinematics with the host galaxy
properties, we find that AGNs with strong outflows have higher star formation
rate and higher HI gas fraction than those AGNs with weak outflows. These
results suggest that the current feedback from AGN-driven outflows do not
instantaneously suppress or quench the star formation in the host galaxies
while its effect is delayed.
