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We analyse the surface brightness profiles of disc-type galaxies in the EAGLEsimulations in order to investigate the effects of galaxy mass and environmenton galaxy profile types. Following observational works, we classify thesimulated galaxies by their disc surface brightness profiles into singleexponential (Type I), truncated (Type II) and anti-truncated (Type III)profiles. In agreement with previous observation and theoretical work, we findthat Type II discs result from truncated star-forming discs that drive radialgradients in the stellar populations. In contrast, Type III profiles resultfrom galaxy mergers, extended star-forming discs or the late formation of asteeper, inner disc. We find that the EAGLE simulations qualitatively reproducethe observed trends found between profile type frequency and galaxy mass,morphology and environment, such as the fraction of Type III galaxiesincreasing with galaxy mass, and the the fraction of Type II galaxiesincreasing with Hubble type. We investigate the lower incidence of Type IIgalaxies in galaxy clusters, finding, in a striking similarity to observedgalaxies, that almost no S0-like galaxies in clusters have Type II profiles.Similarly, the fraction of Type II profiles for disc-dominated galaxies inclusters is significantly decreased relative to field galaxies. This differencebetween field and cluster galaxies is driven by star formation quenching.Following the cessation of star formation upon entering a galaxy cluster, theyoung stellar populations of Type II galaxies simply fade, leaving behind TypeI galaxies.

Using the EAGLE simulations to elucidate the origin of disc surface brightness profile breaks as a function of mass and environment