Dynamical Delays Between Starburst and AGN Activity in Galaxy Nuclei

TL;DR

This paper proposes a dynamical explanation for the observed delay between starburst and AGN activity in galaxy nuclei, emphasizing the role of gas dynamics and gravitational torques rather than feedback mechanisms.

Contribution

It introduces a new dynamical model showing that delays between star formation and AGN activity can naturally arise in bright quasars due to gas inflow and gravitational effects.

Findings

Delay between starburst and AGN peaks can be 10-100 local dynamical times.

Gas supply in mergers can be effectively infinite, allowing prolonged BH growth.

Delay varies with the radius over which star formation is measured.

Abstract

Observations of AGN have suggested a possible delay between the peak of star formation (on some scale) and AGN activity. Inefficient fueling (and/or feedback) from fast stellar winds has been invoked to explain this, but we argue this is unlikely in bright systems accreting primarily cold dense gas. We show that such a delay can arise even in bright quasars for purely dynamical reasons. If some large-scale process produces rapid inflow, smaller scales will quickly become gas-dominated. As the gas density peaks, so does the SFR. However, gravitational torques which govern further inflow are relatively inefficient in gas-dominated systems; as more gas is turned into stars, the stars provide an efficient angular momentum sink allowing more rapid inflow. Moreover, the gas provided to the central regions in mergers or strong disk instabilities will typically be ~100 times larger than that needed to fuel the BH; the system is effectively in the 'infinite gas supply' limit. BH growth can therefore continue for some time while the gas supply exhausts, until it has significantly depleted to the point where the BH is finally 'starved.' Both of these effects act together with comparable magnitude, and mean that the peak of BH growth can lag the peak in the SFR measured at a given scale by a timescale corresponding to the gas exhaustion time on that scale (~ 10-100 local dynamical times). This predicts that the inferred delay will vary in a specific manner with the radius over which the star formation rate is measured. We discuss possible implications for the role of AGN feedback in suppressing star formation activity.