Chandra survey of nearby highly inclined disk galaxies -- IV: New insights into the working of stellar feedback

TL;DR

This study examines how stellar feedback influences the hot gas emission in nearby disk galaxies, revealing complex relationships between star formation activity, galaxy mass, and coronal X-ray emission, challenging previous assumptions.

Contribution

It provides new empirical insights into the dependence of galactic coronal emission efficiency on star formation rates and galaxy parameters, highlighting the nuanced role of stellar feedback.

Findings

Coronal X-ray luminosity correlates sub-linearly with specific SFR.

Emission efficiency decreases with increasing surface SFR.

The plasma temperature weakly correlates with surface SFR.

Abstract

Galaxy evolution is regulated by the interplay between galactic disks and their surrounding medium. We study this interplay by examining how the galactic coronal emission efficiency of stellar feedback depends on the (surface and specific) star formation rates (SFRs) and other parameters for a sample of 52 Chandra-observed nearby highly inclined disk galaxies. We first measure the star forming galactic disk sizes, as well as the SFRs of these galaxies, using data from the Wide-Field Infrared Survey Explorer, and then show that 1) the specific 0.5-2~keV luminosity of the coronal emission correlates with the specific SFR in a {\sl sub-linear} fashion: on average, $L_X/L_K \propto (SFR/M_*)^{\Gamma}$ with $\Gamma =0.29\pm0.12$; 2) the efficiency of the emission $ L_X/SFR$ decreases with increasing surface SFR ($I_{SFR}$; $\Gamma = -0.44\pm0.12$); and 3) the characteristic temperature of the X-ray-emitting plasma weakly correlates with $I_{SFR}$ ($\Gamma = 0.08\pm0.04$). These results, somewhat surprising and anti-intuitive, suggest that a) the linear correlation between $L_X$ and SFR, as commonly presented, is largely due to the correlation of these two parameters with galaxy mass; b) much of the mechanical energy from stellar feedback likely drives global outflows with little X-ray cooling and with a mass-loading efficiency decreasing fast with increasing $I_{SFR}$ ($\Gamma \lesssim -0.5$); c) these outflows heat and inflate the medium around the galactic disks of massive galaxies, reducing its radiative cooling rate, whereas for relatively low-mass galaxies, the energy in the outflows is probably dissipated in regions far away from the galactic disks.