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We have evaluated the diffuse intracluster light (ICL) in the central core ofthe galaxy cluster CL0024+17 at $z\sim 0.4$ observed with the prime focuscamera (LBC) at LBT. The measure required an accurate removal of the galaxieslight within $\sim 200$ kpc from the center. The residual background intensityhas then been integrated in circular apertures to derive the average ICLintensity profile. The latter shows an approximate exponential decline asexpected from theoretical cold dark matter models. The radial profile of theICL over the galaxies intensity ratio (ICL fraction) is increasing withdecreasing radius but near the cluster center it starts to bend and thendecreases where the overlap of the halos of the brightest cluster galaxiesbecomes dominant. Theoretical expectations in a simplified CDM scenario showthat the ICL fraction profile can be estimated from the stripped over galaxystellar mass ratio in the cluster. It is possible to show that the latterquantity is almost independent of the properties of the individual hostgalaxies but mainly depends on the average cluster properties. The predictedICL fraction profile is thus very sensitive to the assumed CDM profile, totalmass and concentration parameter of the cluster. Adopting values very similarto those derived from the most recent lensing analysis in CL0024+17 we find agood agreement with the observed ICL fraction profile. The galaxy counts in thecluster core have then been compared with that derived from composite clustersamples in larger volumes, up to the clusters virial radius. The galaxy countsin the CL0024+17 core appear flatter and the amount of bending respect to theaverage cluster galaxy counts imply a loss of total emissivity in broadagreement with the measured ICL fraction.

Diffuse optical intracluster light as a measure of stellar tidal stripping: the cluster CL0024+17 at $z\sim $0.4 observed at LBT