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We study the distribution of the Milky Way satellites stellar and dark matterdebris. For the first time we address the question of the tidal disruption ofsatellites in simulations by utilising simultaneously a) a realistic set oforbits extracted from cosmological simulations, b) a three component hostgalaxy with live halo, disc and bulge components, and c) satellites fromhydrodynamical simulations. We analyse the statistical properties of thesatellite debris of all massive galaxies reaching the inner Milky Way on atimescale of 2 Gyr. Up to 80$\%$ of the dark matter is stripped from thesatellites, while this happens for up to 30$\%$ of their stars. The stellardebris ends mostly in the inner Milky Way halo, whereas the dark matter debrisshows a flat mass distribution over the full main halo. The dark matter debrisfollows 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 debrisis flatter than that of the dark matter debris and the orientations of theirshort axes differ significantly. Changing the orientation of the stellar discby 90$^{\rm{o}}$ has only a minor impact on the distribution of the satellitedebris. Our results indicate that the dark matter is more easily stripped thanstars from the Milky Way satellites. The structure of the debris is dominatedby the satellite orbital properties. The radial profiles, the flattening andthe orientation of the stellar and dark matter debris are significantlydifferent, which prevents the prediction of the dark matter distribution fromthe observed stellar component.

Addressing via N-body simulations the distribution of the satellite tidal debris in the Milky Way environment