The formation of low metallicity globular clusters in dwarf galaxy
  mergers
  We present a hydro-dynamical simulation at sub-parsec and few solar mass
resolution of a merger between two gas-rich dwarf galaxies. Our simulation
includes a detailed model for the multi-phase interstellar medium (ISM) and is
able to follow the entire formation history of spatially resolved star
clusters, including feedback from individual massive stars. Shortly after the
merger we find a population of $\sim 900$ stellar clusters with masses above
$10^{2.5}\; \rm{M_\odot}$ and a cluster mass function (CMF), which is well
fitted with a power-law with a slope of $\alpha=-1.70\pm0.08$. We describe here
in detail the formation of the three most massive clusters (M$_{*} \gtrsim
10^5$ M$_\odot$), which populate the high-mass end of the CMF. The simulated
clusters form rapidly on a timescale of $6$-$8$ Myr in converging flows of
dense gas. The embedded merger phase has extremely high star formation rate
surface densities of $\Sigma_\mathrm{SFR}>10\; \mathrm{M}_\odot\;
\mathrm{yr}^{-1}\; \mathrm{kpc}^{-2}$ and thermal gas pressures in excess of
$P_{\rm th}\sim10^7 \; \mathrm{k}_{\rm B}\;(\rm K\;\mathrm{cm}^{-3})^{-1}$. The
formation process is terminated by rapid gas expulsion driven by the first
generation of supernovae, after which the cluster centers relax and both their
structure and kinematics become indistinguishable from observed local globular
clusters. The simulation presented here provides a general model for the
formation of metal-poor globular clusters in chemically unevolved starbursting
environments of low-mass dwarf galaxies, which are common at high redshifts.
