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Dust attenuation varies substantially from galaxy to galaxy and as of yetcannot be reproduced from first principles in theoretical models. In Nagaraj etal. (2022), we developed the first Bayesian population model of dustattenuation as a function of stellar population properties and projected galaxyshape, built on spectral energy distribution (SED) fits of nearly 30,000galaxies in the 3D-HST grism survey with broadband photometric coverage fromthe rest-frame UV to IR. In this paper, we apply the model to galaxies from thelarge-volume cosmological simulation TNG100. We produce a UVJ diagram andcompare it with one obtained in previous work by applying approximate radiativetransfer to the simulated galaxies. We find that the UVJ diagram based on ourempirical model is in better agreement with observations than the previouseffort, especially in the number density of dusty star forming galaxies. Wealso construct the intrinsic dust-free UVJ diagram for TNG and 3D-HST galaxiesat z ~ 1, finding qualitative agreement but residual differences at the 10-20%level. These differences can be largely attributed to the finding that TNGgalaxies have, on average, 29% younger stellar populations and 0.28 dex highermetallicities than observed galaxies.

Empirical Dust Attenuation Model Leads to More Realistic UVJ Diagram for TNG100 Galaxies