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We study three cosmological hydrodynamical simulations of Milky Way(MW)-sizedhalos including a comparison with the dark matter(DM)-only counterparts. Wefind one of our simulated galaxies with interesting MW-like features. Thanks toa consistently tuned star formation rate and supernovae feedback we obtain anextended disk and a flat rotation curve with a satisfying circular velocity anda reasonable DM density in the solar neighbourhood. Mimicking observationalmethods, we re-derive the stellar mass and obtain stellar-to-halo mass ratiosreduced by more than 50\%. We show the interaction between the baryons and thedark matter which is first contracted by star formation and then cored byfeedback processes. Indeed, we report an unprecedentedly observed effect in theDM density profile consisting of a central core combined with an adiabaticcontraction at larger galactic radii. The cores obtained are typically $\sim$ 5kpc large. Moreover, this also impacts the DM density at the solar radius. Inour simulation resembling most to the MW, the density is raised from 0.23GeV/cm$^3$ in the dark matter only run to 0.36 GeV/cm$^3$ (spherical shell) or0.54 GeV/cm$^3$ (circular ring) in the hydrodynamical run. Studying thesubhalos, the dark matter within luminous satellites is also affected bybaryonic processes and exihibits cored profiles whereas dark satellites arecuspy. We find a shift in mass compared to DM-only simulations and obtain, forhalos in the lower MW mass range, a distribution of luminous satellitescomparable to the MW spheroidal dwarf galaxies.

Baryonic and dark matter distribution in cosmological simulations of spiral galaxies