  We present detailed radiative transfer simulations of the reionization
history of the Milky Way by metal-poor globular clusters. We identify potential
metal-poor globular cluster candidates within the Aquarius simulation using
dark matter halo velocity dispersions. We calculate the local ionization fields
via a photon-conserving, three dimensional non-equilibrium chemistry code and
allow the model to propagate through to the present day. The key feature of the
model is that globular cluster formation is suppressed if the local gas is
ionized.
  We find that our spatial treatment of the ionization field leads to
drastically different numbers and spatial distributions when compared to models
where globular cluster formation is simply truncated at a given redshift. We
find that it is possible for metal-poor globular clusters to have formed via
the dark matter halo formation channel as our secondary model (delayed
formation) combined with truncation at z = 10 produces radial distributions
statistically consistent with that of the Milky Way metal-poor globular
clusters.
  If globular clusters do indeed form within high-redshift dark matter halos,
if only in-part, their contributions to the reionization of the local (i.e. 2^3
h^-3 Mpc^3 centred on the host galaxy) volume and mass by redshift 10 could be
as high as 98% and 90%, respectively. In our photon poorest model, this
contribution drops to 60% and 50%. The surviving clusters in all models have a
narrow average age range (mean = 13.34 Gyr, \sigma = 0.04 Gyr) consistent with
current ages estimates of the Milky Way metal-poor globular clusters.
  We also test a simple dynamical destruction model and estimate that ~60% of
all metal-poor globular clusters formed at high redshift have since been
destroyed via tidal interactions with the host galaxy.
