2015MNRAS.454.1886S

We study how optical galaxy morphology depends on mass and star formation rate (SFR) in the Illustris Simulation. To do so, we measure automated galaxy structures in 10808 simulated galaxies at z = 0 with stellar masses 109.7 < M*/M_☉ < 1012.3. We add observational realism to idealized synthetic images and measure non-parametric statistics in rest-frame optical and near-IR images from four directions. We find that Illustris creates a morphologically diverse galaxy population, occupying the observed bulge strength locus and reproducing median morphology trends versus stellar mass, SFR, and compactness. Morphology correlates realistically with rotation, following classification schemes put forth by kinematic surveys. Type fractions as a function of environment agree roughly with data. These results imply that connections among mass, star formation, and galaxy structure arise naturally from models matching global star formation and halo occupation functions when simulated with accurate methods. This raises a question of how to construct experiments on galaxy surveys to better distinguish between models. We predict that at fixed halo mass near 10¹²M_☉, disc-dominated galaxies have higher stellar mass than bulge-dominated ones, a possible consequence of the Illustris feedback model. While Illustris galaxies at M* ∼ 10¹¹M_☉ have a reasonable size distribution, those at M* ∼ 10¹⁰M_☉ have half-light radii larger than observed by a factor of 2. Furthermore, at M* ∼ 10^10.5-10¹¹M_☉, a relevant fraction of Illustris galaxies have distinct `ring-like' features, such that the bright pixels have an unusually wide spatial extent.