  We study the optical morphology of galaxies in a large-scale hydrodynamic
cosmological simulation, the EAGLE simulation. Galaxy morphologies were
characterized using non-parametric statistics (Gini, $M_{20}$, Concentration
and Asymmetry) derived from mock images computed using a 3D radiative transfer
technique and post-processed to approximate observational surveys. The
resulting morphologies were contrasted to observational results from a sample
of $\log_{10}(M_{*}/M_\odot) > 10$ galaxies at $z \sim 0.05$ in the GAMA
survey. We find that the morphologies of EAGLE galaxies reproduce observations,
except for asymmetry values which are larger in the simulated galaxies.
Additionally, we study the effect of spatial resolution in the computation of
non-parametric morphologies, finding that Gini and Asymmetry values are
systematically reduced with decreasing spatial resolution. Gini values for
lower mass galaxies are especially affected. Comparing against other large
scale simulations, the non-parametric statistics of EAGLE galaxies largely
agree with those found in IllustrisTNG. Additionally, EAGLE galaxies mostly
reproduce observed trends between morphology and star formation rate and galaxy
size. Finally, We also find a significant correlation between optical and
kinematic estimators of morphologies, although galaxy classification based on
an optical or a kinematic criteria results in different galaxy subsets. The
correlation between optical and kinematic morphologies is stronger in central
galaxies than in satellites, indicating differences in morphological evolution.
