The Lowest Metallicity Stars in the LMC: Clues from MaGICC Simulations
  Using a cosmological hydrodynamical simulation of a galaxy of similar mass to
the Large Magellanic Cloud (LMC), we examine the predicted characteristics of
its lowest metallicity populations. In particular, we emphasise the spatial
distributions of first (Pop III) and second (polluted by only immediate Pop III
ancestors) generation stars. We find that primordial composition stars form not
only in the central galaxy's progenitor, but also in locally collapsed
sub-halos during the early phases of galaxy formation. The lowest metallicity
stars in these sub-halos end up in a relatively extended distribution around
the host, with these accreted stars possessing present-day galactocentric
distances as great as ~40kpc. By contrast, the earliest stars formed within the
central galaxy remain in the inner region, where the vast majority of star
formation occurs, for the entirety of the simulation. Consequently, the
fraction of stars that are from the earliest generation increases strongly with
radius.
