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The galaxy distribution in dark matter-dominated halos is expected toapproximately trace the details of the underlying dark matter substructure. Inthis paper we introduce halo `core-tracking' as a way to efficiently follow thesmall-scale substructure in cosmological simulations and apply the technique tomodel the galaxy distribution in observed clusters. The method relies onexplicitly tracking the set of particles identified as belonging to a halo'scentral density core, once a halo has attained a certain threshold mass. Thehalo cores are then followed throughout the entire evolution of the simulation.The aim of core-tracking is to simplify substructure analysis tasks by avoidingthe use of subhalos and, at the same time, to more easily account for theso-called ``orphan'' galaxies, which have lost substantial dark mass due totidal stripping. We show that simple models based on halo cores can reproducethe number and spatial distribution of galaxies found in optically-selectedclusters in the Sloan Digital Sky Survey. We also discuss future applicationsof the core-tracking methodology in studying the galaxy-halo connection.

Modeling the Galaxy Distribution in Clusters using Halo Cores