Baryonic and dark matter distribution in cosmological simulations of
  spiral galaxies
  We study three cosmological hydrodynamical simulations of Milky Way(MW)-sized
halos including a comparison with the dark matter(DM)-only counterparts. We
find one of our simulated galaxies with interesting MW-like features. Thanks to
a consistently tuned star formation rate and supernovae feedback we obtain an
extended disk and a flat rotation curve with a satisfying circular velocity and
a reasonable DM density in the solar neighbourhood. Mimicking observational
methods, we re-derive the stellar mass and obtain stellar-to-halo mass ratios
reduced by more than 50\%. We show the interaction between the baryons and the
dark matter which is first contracted by star formation and then cored by
feedback processes. Indeed, we report an unprecedentedly observed effect in the
DM density profile consisting of a central core combined with an adiabatic
contraction at larger galactic radii. The cores obtained are typically $\sim$ 5
kpc large. Moreover, this also impacts the DM density at the solar radius. In
our simulation resembling most to the MW, the density is raised from 0.23
GeV/cm$^3$ in the dark matter only run to 0.36 GeV/cm$^3$ (spherical shell) or
0.54 GeV/cm$^3$ (circular ring) in the hydrodynamical run. Studying the
subhalos, the dark matter within luminous satellites is also affected by
baryonic processes and exihibits cored profiles whereas dark satellites are
cuspy. We find a shift in mass compared to DM-only simulations and obtain, for
halos in the lower MW mass range, a distribution of luminous satellites
comparable to the MW spheroidal dwarf galaxies.
