  By using deep observations of clusters of galaxies, it has been recently
found that the projected stellar mass density closely follows the projected
total (dark and baryonic) mass density within the innermost ~140 kpc. In this
work, we aim to test these observations using the Cluster-EAGLE simulations,
comparing the projected densities inferred directly from the simulations. We
compare the iso-density contours using the procedure of Montes \& Trujillo
(2019), and find that the shape of the stellar mass distribution follows that
of the total matter even more closely than observed, although their radial
profiles differ substantially. The ratio between stellar and total matter
density profiles in circular apertures, shows a slope close to -1, with a small
dependence on the cluster's total mass. We propose an indirect method to
calculate the halo mass and mass density profile from the radial profile of the
intra-cluster stellar mass density.
