Effects of Stellar Feedback on Stellar and Gas Kinematics of Star-Forming Galaxies at 0.6<z<1.0

TL;DR

This study investigates how stellar feedback influences the kinematics of stars and gas in star-forming galaxies at redshifts 0.6 to 1.0, providing observational evidence supporting simulation predictions about dark matter profile flattening.

Contribution

It offers the first observational validation of the correlation between velocity dispersions and star formation rate predicted by cosmological simulations.

Findings

Weak but significant correlation between velocity dispersions and sSFR in low-mass galaxies.

Correlation strength increases with redshift.

Supports feedback-driven outflows affecting dark matter profiles.

Abstract

Recent zoom-in cosmological simulations have shown that stellar feedback can flatten the inner density profile of the dark matter halo in low-mass galaxies. A correlation between the stellar/gas velocity dispersion ($\sigma_{star}$, $\sigma_{gas}$) and the specific star formation rate (sSFR) is predicted as an observational test of the role of stellar feedback in re-shaping the dark matter density profile. In this work we test the validity of this prediction by studying a sample of star-forming galaxies at $0.6<z<1.0$ from the LEGA-C survey, which provides high signal-to-noise measurements of stellar and gas kinematics. We find that a weak but significant correlation between $\sigma_{star}$ (and $\sigma_{gas}$) and sSFR indeed exists for galaxies in the lowest mass bin (M$_\ast\sim10^{10}\,$M$_\odot$). This correlation, albeit with a $\sim$35% scatter, holds for different tracers of star formation, and becomes stronger with redshift. This result generally agrees with the picture that at higher redshifts star formation rate was generally higher, and galaxies at M$_\ast\lesssim10^{10}\,$M$_\odot$ have not yet settled into a disk. As a consequence, they have shallower gravitational potentials more easily perturbed by stellar feedback. The observed correlation between $\sigma_{star}$ (and $\sigma_{gas}$) and sSFR supports the scenario predicted by cosmological simulations, in which feedback-driven outflows cause fluctuations in the gravitation potential that flatten the density profiles of low-mass galaxies.