  The dividing line between galaxies that are quenched by reionization
("relics") and galaxies that survive reionization (i.e. continue forming stars)
is commonly discussed in terms of a halo mass threshold. We probe this
threshold in a physically more complete and accurate way than has been possible
to date, using five extremely high resolution ($M_\mathrm{target}=4M_\odot$)
cosmological zoom-in simulations of dwarf galaxies within the halo mass range
$1-4\times10^9M_\odot$. The employed LYRA simulation model features resolved
interstellar medium physics and individual, resolved supernova explosions. In
our results, we discover an interesting intermediate population of dwarf
galaxies close to the threshold mass but which are neither full reionization
relics nor full reionization survivors. These galaxies initially quench at the
time of reionization but merely remain quiescent for ~500Myr. At $z\approx5$
they recommence star formation in a synchronous way, and remain star-forming
until the present day. These results demonstrate that the halo mass at $z=0$ is
not a good indicator of survival close to the threshold. While the star
formation histories we find are diverse, we show that they are directly related
to the ability of a given halo to retain and cool gas. Whereas the latter is
most strongly dependent on the mass (or virial temperature) of the host halo at
the time of reionization, it also depends on its growth history, the UV
background (and its decrease at late times) and the amount of metals retained
within the halo.
