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The EAGLE simulation suite has previously been used to investigate therelationship between the stellar mass of galaxies, $M_{*}$, and the propertiesof dark matter halos, using the hydrodynamical reference simulation combinedwith a dark matter only (DMO) simulation having identical initial conditions.The stellar masses of central galaxies in halos with $M_{\mathrm{200c}} >10^{11} \mathrm{M_{\odot}}$ were shown to correlate with the DMO halo maximumcircular velocity, with $\approx 0.2$ dex of scatter that is uncorrelated withother DMO halo properties. Here we revisit the origin of the scatter in the$M_{*}-V_{\mathrm{max, DMO}}$ relation in EAGLE at $z = 0.1$. We find that thescatter in $M_{*}$ correlates with the mean age of the galaxy stellarpopulation such that more massive galaxies at fixed $V_{\mathrm{max, DMO}}$ areyounger. The scatter in the stellar mass and mean stellar population ageresults from variation in the baryonic mass, $M_{\mathrm{bary}} =M_{\mathrm{gas}} + M_{*}$, of the galaxies' progenitors at fixed halo mass andconcentration. At the redshift of peak correlation ($z \approx 1$), theprogenitor baryonic mass accounts for $75\%$ of the variance in the $z=0.1$$M_{*}-V_{\mathrm{max, DMO}}$ relation. The scatter in the baryonic mass, inturn, is primarily set by differences in feedback strength and gas accretionover the course of the evolution of each halo.

The evolution of the baryon fraction in halos as a cause of scatter in the galaxy stellar mass in the EAGLE simulation