  The role of baryonic physics, star formation, and stellar feedback, in
shaping the galaxies and their host halos is an evolving topic. The dark matter
aspects are illustrated in this work by showing distribution features in a
Milky-Way-sized halo. We focus on the halo morphology, geometry, and profile as
well as the phase space distribution using one dark matter only and five
hydrodynamical cosmological high-resolution simulations of the same halo with
different subgrid prescriptions for the baryonic physics (Kennicut versus
multi-freefall star formation and delayed cooling versus mechanical supernovae
feedback). If some general properties like the relative halo-galaxy orientation
are similar, the modifications of the gravitational potential due to the
presence of baryons are found to induce different dark matter distributions
(rounder and more concentrated halo). The mass density profile as well as the
velocity distribution are modified distinctively according to the specific
resulting baryonic distribution highlighting the variability of those
properties (e.g inner power index from 1.3 to 1.8, broader speed distribution).
The uncertainties on those features are of paramount importance for dark matter
phenomenology, particularly when dealing with dark matter dynamics or direct
and indirect detection searches. As a consequence, dark matter properties and
prospects using cosmological simulations require improvement on baryonic
physics description. Modeling such processes is a key issue not only for galaxy
formation but also for dark matter investigations.
