Primordial Gas Collapse in The Presence of Radiation: Direct Collapse
  Black Hole or Population III star?
  The first billion years in the evolution of the Universe mark the formation
of the first stars, black holes and galaxies. The radiation from the first
galaxies plays an important role in determining the final state of primordial
gas collapsing in a neighboring halo. This is due to the fact that the primary
coolant for primordial gas is molecular hydrogen, which can be dissociated into
atomic hydrogen by Lyman-Werner photons in the energy range $11.2 - 13.6$~eV.
While cooling by molecular hydrogen leads to Pop. III star formation, cooling
by atomic hydrogen can lead to the formation of a supermassive star (or
quasi-star) which results in the formation of a massive $10^{4-5} M_\odot$
black hole, or a direct collapse black hole. The spectrum of this radiation
field is critical in order to determine whether a primordial gas cloud forms a
Pop. III star or a very massive black hole. We will in the following explore
this scenario and discuss how the radiation spectrum influences the outcome of
the collapse.
