What drives the evolution of gas kinematics in star-forming galaxies?

TL;DR

This study uses FIRE cosmological simulations to explore the drivers of increased gas velocity dispersion in star-forming galaxies, revealing that gas inflow and star formation are closely linked to kinematic evolution across cosmic time.

Contribution

It demonstrates that gas inflow and star formation rate fluctuations are key drivers of velocity dispersion evolution, aligning simulation results with observational trends.

Findings

Velocity dispersion correlates with SFR in both observations and simulations.

Velocity dispersion increases with redshift up to z~1, then flattens.

Gas inflow rate variations closely match changes in velocity dispersion and SFR.

Abstract

One important result from recent large integral field spectrograph (IFS) surveys is that the intrinsic velocity dispersion of galaxies traced by star-forming gas increases with redshift. Massive, rotation-dominated discs are already in place at z~2, but they are dynamically hotter than spiral galaxies in the local Universe. Although several plausible mechanisms for this elevated velocity dispersion (e.g. star formation feedback, elevated gas supply, or more frequent galaxy interactions) have been proposed, the fundamental driver of the velocity dispersion enhancement at high redshift remains unclear. We investigate the origin of this kinematic evolution using a suite of cosmological simulations from the FIRE (Feedback In Realistic Environments) project. Although IFS surveys generally cover a wider range of stellar masses than in these simulations, the simulated galaxies show trends between intrinsic velocity dispersion, SFR, and redshift in agreement with observations. In both the observed and simulated galaxies, intrinsic velocity dispersion is positively correlated with SFR. Intrinsic velocity dispersion increases with redshift out to z~1 and then flattens beyond that. In the FIRE simulations, intrinsic velocity dispersion can vary significantly on timescales of <100 Myr. These variations closely mirror the time evolution of the SFR and gas inflow rate. By cross-correlating pairs of intrinsic velocity dispersion, gas inflow rate, and SFR, we show that increased gas inflow leads to subsequent enhanced star formation, and enhancements in intrinsic velocity dispersion tend to temporally coincide with increases in gas inflow rate and SFR.