Dark Matter Response to Galaxy Assembly History
  Aims: It is well known that the presence of baryons affects the dark matter
host haloes. Exploring the galaxy assembly history together with the dark
matter haloes properties through time can provide a way to measure these
effects. Methods: We study the properties of four Milky Way mass dark matter
haloes from the Aquarius project during their assembly history, between $z = 0
- 4$. In this work, we use the SPH run from Scannapieco et al. (2009) and the
dark matter only counterpart as case studies. To asses the robustness of our
findings, we compare them with one of the haloes run using a moving-mesh
technique and different sub-grid scheme. Results: Our results show that the
cosmic evolution of the dark matter halo profiles depends on the assembly
history of the baryons. We find that the dark matter profiles do not
significantly change with time, hence they become stable, when the fraction of
baryons accumulated in the central regions reaches 80 percent of its present
mass within the virial radius. Furthermore, the mass accretion history shows
that the haloes that assembled earlier are those that contain a larger amount
of baryonic mass aforetime, which in turn allows the dark matter halo profiles
to reach a stable configuration earlier. For the SPH haloes, we find that the
specific angular momentum of the dark matter particles within the five percent
of the virial radius at z = 0, remains approximately constant from the time at
which 60 percent of the stellar mass is gathered. We explore different
theoretical and empirical models for the contraction of the haloes through
redshift. A model to better describe the contraction of the haloes through
redshift evolution must depend on the stellar mass content in the inner
regions.
