  We describe our new "MLAPM-halo-finder" (MHF) which is based on the adaptive
grid structure of the N-body code MLAPM. We then extend the MHF code in order
to track the orbital evolution of gravitationally bound objects through any
given cosmological N-body simulation - our so-called "MLAPM-halo-tracker"
(MHT). The mode of operation of MHT is demonstrated using a series of eight
high-resolution N-body simulations of galaxy clusters. Each of these halos
hosts more than one million particles within their virial radii Rvir. We use
MHT as well as MHF to follow the temporal evolution of hundreds of individual
satellites, and show that the radial distribution of these substructure
satellites follows a "universal" radial distribution irrespective of the host
halo's environment and formation history. This in fact might pose another
problem for simulations of CDM structure formation as there are recent findings
by Taylor et al. (2003) that the Milky Way satellites are found preferentially
closer to the galactic centre and simulations underestimate the amount of
central substructure, respectively. Further, this universal substructure
profile is anti-biased with respect to the underlying dark matter profile. Both
the halo finder MHF and the halo tracker MHT will become part of the open
source MLAPM distribution.
