Balmer beaks and rest-frame Hα EWs of model galaxies that halted star formation at a grid of times before observation. The Bagpipes models assume a constant SFH of 100 Myr before star formation is stopped. They were computed with three different metallicities and two dust scenarios: A_V = 0 and A_V = 0.8. The gray region denotes the parameter space from which galaxies were selected for our sample. We find that the evolution of the Balmer breaks is metallicity- and dust-dependent, while Hα EWs experience minimal variations between different metallicities, with no variations with different dust attenuation since we applied the same dust screen to the nebular lines as to the continuum.