The distribution of mass components in simulated disc galaxies
  Using 22 hydrodynamical simulated galaxies in a LCDM cosmological context we
recover not only the observed baryonic Tully-Fisher relation, but also the
observed "mass discrepancy--acceleration" relation, which reflects the
distribution of the main components of the galaxies throughout their disks.
This implies that the simulations, which span the range 52 < V$_{\rm flat}$ <
222 km/s where V$_{\rm flat}$ is the circular velocity at the flat part of the
rotation curve, and match galaxy scaling relations, are able to recover the
observed relations between the distributions of stars, gas and dark matter over
the radial range for which we have observational rotation curve data.
Furthermore, we explicitly match the observed baryonic to halo mass relation
for the first time with simulated galaxies. We discuss our results in the
context of the baryon cycle that is inherent in these simulations, and with
regards to the effect of baryonic processes on the distribution of dark matter.
