  The formation of satellite systems in circum-planetary discs is considered to
be similar to the formation of rocky planets in a proto-planetary disc,
especially Super-Earths. Thus, it is possible to use systems with large
satellites to test formation theories that are also applicable to extrasolar
planets. Furthermore, a better understanding of the origin of satellites might
yield important information about the environment near the growing planet
during the last stages of planet formation. In this work we investigate the
formation and migration of the Jovian satellites through N-body simulations. We
simulated a massive, static, low viscosity, circum-planetary disc in agreement
with the minimum mass sub-nebula model prescriptions for its total mass. In
hydrodynamic simulations we found no signs of gaps, therefore type II migration
is not expected. Hence, we used analytic prescriptions for type I migration,
eccentricity and inclination damping, and performed N-body simulations with
damping forces added. Detailed parameter studies showed that the number of
final satellites is strong influenced by the initial distribution of embryos,
the disc temperature, and the initial gas density profile. For steeper initial
density profiles it is possible to form systems with multiple satellites in
resonance while a flatter profile favours the formation of satellites close to
the region of the Galilean satellites. We show that the formation of massive
satellites such as Ganymede and Callisto can be achieved for hotter discs with
an aspect ratio of H/r ~ 0.15 for which the ice line was located around 30 R_J.
