  Partially obscured AGNs within a redshift range $z=0.011\sim0.256$ are used
to re-study the role of feedback in the AGN-host coevolution issue in terms of
their [OIII]$\lambda$5007 emission line profile. The spectra of these objects
enable us to determine the AGN's accretion properties directly from their broad
H$\alpha$ emission. This is essential for getting rid of the "circular
reasoning" in our previous study of narrow emission-line galaxies, in which the
[OIII] emission line was used not only as a proxy of AGN's bolometric
luminosity, but also as a diagnostic of outflow. In addition, the measurement
of $D_n(4000)$ index is improved by removing an underlying AGN's continuum
according to the corresponding broad H$\alpha$ emission. With these
improvements, we confirm and reinforce the correlation between
$L/L_{\mathrm{Edd}}$ and stellar population age. More important is that this
correlation is found to be related to both [OIII] line blue asymmetry and bulk
blueshift velocity, which suggests a linkage between SMBH growth and host star
formation through the feedback process. The current sample of partially
obscured AGNs shows that the composite galaxies have younger host stellar
population, higher Eddington ratio, less significant [OIII] blue wing and
smaller bulk [OIII] line shift than do the Seyfert galaxies .
