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In the standard paradigm, satellite galaxies are believed to be associatedwith the population of dark matter subhalos. In this paper, we use theconditional stellar mass functions of {\it satellite galaxies} obtained from alarge galaxy group catalogue together with models of the subhalo mass functionsto explore the fraction and fate of stripped stars from satellites in galaxygroups and clusters of different masses. The majority of the stripped stars inmassive halos are predicted to end up as intra-cluster stars, and the predictedamounts of the intra-cluster component as a function of the velocity dispersionof galaxy system match well the observational results obtained by Gonzalez etal. (2007). The fraction of the mass in the stripped stars to that remain boundin the central and satellite galaxies is the highest ($\sim 40%$ of the totalstellar mass) in halos with masses $M_h\sim 10^{14}\msunh$. If all these starsend up in the intra-cluster component (Max), or maximum of them are accretedinto the central galaxy (Min), then we can predict that a maximum $\sim 19%$and a minimum $\sim 5%$ of the total stars in the whole universe are in termsof the diffused intra-cluster component. In the former case, in massive haloswith $M_h \sim 10^{15} \msunh$, the stellar mass of the intra-cluster componentis roughly 6 times as large as that of the central galaxy. This factordecreases to $\sim 2$, 1 and 0.1 in halos with $M_h \sim 10^{14}$, $10^{13}$,and $10^{12} \msunh$, respectively. The total amount of stars stripped fromsatellite galaxies is insufficient to build up the central galaxies in haloswith masses $\la 10^{12.5}\msunh$, and so the quenching of star formation mustoccur in halos with higher masses. Abridged.

The subhalo - satellite connection and the fate of disrupted satellite galaxies