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We investigate on the role of the halo concentration in the formation of theintra-cluster light (ICL) in galaxy groups and clusters, as predicted by astate-of-art semi-analytic model of galaxy formation, coupled with a set ofhigh-resolution dark matter only simulations. The analysis focuses on how thefraction of ICL correlates with halo mass, concentration and fraction ofearly-type galaxies (ETGs) in a large sample of groups and clusters with$13.0\leq \log M_{halo} \leq 15.0$. The fraction of ICL follows a normaldistribution, a consequence of the stochastic nature of the physical processesresponsible for the formation of the diffuse light. The fractional budget ofICL depends on both halo mass (very weakly) until group scales, andconcentration (remarkably). More interestingly, the ICL fraction is higher inmore concentrated objects, a result of the stronger tidal forces acting in theinnermost regions of the haloes where the concentration is the quantity playingthe most relevant role. Our model predictions do not show any dependencebetween the ICL and ETGs fractions and so, we instead suggest the concentrationrather than the mass, as recently claimed, to be the main driver of the ICLformation. The diffuse light starts to form in groups via stellar stripping andmergers and later assembled in more massive objects. However, the formation andassembly keep going on group/cluster scales at lower redshift through the sameprocesses, mainly via stellar stripping in the vicinity of the central regionswhere tidal forces are stronger.

The Intracluster Light and its Link with the Dynamical State of the Host Group/Cluster: the Role of the Halo Concentration