  We investigate the connection between ionized gas outflows and star formation
activity using a large sample of type 1 and 2 AGNs with far-IR detections or
star formation rate (SFR) estimates. The strength of ionized gas outflows,
measured by the velocity dispersion and velocity shift of the \OIII\ emission
line, clearly shows a correlation with SFR. The connection between specific
star formation rate (sSFR) and \OIII\ gas velocity dispersion indicates that
AGNs with stronger outflows are hosted by galaxies with higher SFR. Compared to
star-forming galaxies in the main sequence, both type 1 and type 2 AGNs show
sSFR similar to that of non-AGN galaxies, indicating no instantaneous AGN
feedback, while sSFR is higher (lower) for AGNs with stronger (weaker) outflows
than that of main sequence galaxies. These results are consistent with a
delayed AGN feedback scenario. However, it is also possible that a
decease/increase of gas fraction may cause the correlation without AGN
feedback.
