Evolution of massive galaxy properties from their local values out to z ~ 1. The evolution of the dust-mass fraction (M_d∕M_*) was determined from a power-law fit to data from Santini et al. (2014), Béthermin et al. (2015) (for z ≤ 1), and Rémy-Ruyer et al. (2014) for z = 0. The upper bound to the M_d∕M_* evolution is given by assuming M_d ~ 0.5 × Z × M_g, and the evolution of gas and metallicity over this redshift and stellar mass range. The evolution of specific SFR is shaded purple between the relationship in Sargent et al. (2014) and . The evolution of the molecular gas fraction (blue) is from Tacconi et al. (2018). We find that the fraction (F) of dust in clumps surrounding nascent star-forming regions has increased by a factor of ~5.5, and that the overall attenuation of UV (SFR_MS/SFR_UV) has increased by a factor of ~2.5 (ranging from 3.4 to 1.9 for face-on to edge-on galaxies, respectively).