The correlation of outflow kinematics with star formation rate -- Gas outflows in AGNs. VI

TL;DR

This study explores how ionized gas outflows in AGNs relate to star formation rates, revealing correlations that support a delayed feedback scenario but also considering alternative explanations involving gas fraction changes.

Contribution

It provides new observational evidence linking AGN outflow strength with star formation activity, supporting the delayed feedback model in galaxy evolution.

Findings

Ionized gas outflow strength correlates with SFR.

AGNs with stronger outflows have higher sSFR.

Results support a delayed AGN feedback scenario.

Abstract

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.