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We characterise the intra-cluster light (ICL) in ensembles of full-physicscluster simulations from The Three Hundred project, a suite of 324hydrodynamical resimulations of cluster-sized halos. We identify the ICL asthose stellar particles bound to the potential of the cluster itself, but notto any of its substructures, and separate the brightest cluster galaxy (BCG) bymeans of a fixed 50 kpc aperture. We find the total BCG+ICL mass to be inagreement with state-of-the-art observations of galaxy clusters. The ICL massfraction of our clusters is between 30 and 50 per cent of the total stellarmass within $R_{500}$, while the BCG represents around 10 percent. We furtherfind no trend of the ICL fraction with cluster halo mass, at least not in therange $[0.2,3]\cdot10^{15}h^{-1}M_\odot$ considered here. For the dynamicalstate, characterised both by theoretical estimators and by the recent merginghistory of the cluster, there is a clear correlation, such that more relaxedclusters and those that have undergone fewer recent mergers have a higher ICLfraction. Finally, we investigate the possibility of using the ICL to explorethe dark matter (DM) component of galaxy clusters. We compute the volumetricdensity profile for the DM and ICL components and show that, up to $R_{500}$,the ratio between the two can be described by a power law. Working with thevelocity dispersion profiles instead, we show that the ratio can be fit by astraight line. Providing the parameters of these fits, we show how the ICL canbe used to infer DM properties.

Characterising the intra-cluster light in The Three Hundred simulations