Dark matter cores in massive high-$z$ galaxies formed by baryonic clumps
  The rotation curves of some star forming massive galaxies at redshift two
decline over the radial range of a few times the effective radius, indicating a
significant deficit of dark matter (DM) mass in the galaxy centre. The DM mass
deficit is interpreted as the existence of a DM density core rather than the
cuspy structure predicted by the standard cosmological model. A recent study
proposed that a galaxy merger, in which the smaller satellite galaxy is
significantly compacted by dissipative contraction of the galactic gas, can
heat the centre of the host galaxy and help make a large DM core. By using an
$N$-body simulation, we find that a large amount of DM mass is imported to the
centre by the merging satellite, making this scenario an unlikely solution for
the DM mass deficit. In this work, we consider giant baryonic clumps in high
redshift galaxies as alternative heating source for creating the baryon
dominated galaxies with a DM core. Due to dynamical friction, the orbit of
clumps decays in a few Gyr and the baryons condensate at the galactic centre.
As a back-reaction, the halo centre is heated up and the density cusp is
flattened out. The combination of the baryon condensation and core formation
makes the galaxy baryon dominated in the central 2-5 kpc, comparable to the
effective radius of the observed galaxies. Thus, the dynamical heating by giant
baryonic clumps is a viable mechanism for explaining the observed dearth of DM
in high redshift galaxies.
