Addressing via N-body simulations the distribution of the satellite
  tidal debris in the Milky Way environment
  We study the distribution of the Milky Way satellites stellar and dark matter
debris. For the first time we address the question of the tidal disruption of
satellites in simulations by utilising simultaneously a) a realistic set of
orbits extracted from cosmological simulations, b) a three component host
galaxy with live halo, disc and bulge components, and c) satellites from
hydrodynamical simulations. We analyse the statistical properties of the
satellite debris of all massive galaxies reaching the inner Milky Way on a
timescale of 2 Gyr. Up to 80$\%$ of the dark matter is stripped from the
satellites, while this happens for up to 30$\%$ of their stars. The stellar
debris ends mostly in the inner Milky Way halo, whereas the dark matter debris
shows a flat mass distribution over the full main halo. The dark matter debris
follows a density profile with inner power law index $\alpha_{\rm DM}=-0.66$
and outer index $\beta_{\rm DM}=2.94$, while for stars $\alpha_{*}=-0.44$ and
$\beta_{*}=6.17$. In the inner 25 kpc, the distribution of the stellar debris
is flatter than that of the dark matter debris and the orientations of their
short axes differ significantly. Changing the orientation of the stellar disc
by 90$^{\rm{o}}$ has only a minor impact on the distribution of the satellite
debris. Our results indicate that the dark matter is more easily stripped than
stars from the Milky Way satellites. The structure of the debris is dominated
by the satellite orbital properties. The radial profiles, the flattening and
the orientation of the stellar and dark matter debris are significantly
different, which prevents the prediction of the dark matter distribution from
the observed stellar component.
