  Observations of the epoch of reionization give us clues about the nature and
evolution of the sources of ionizing photons, or early stars and galaxies. We
present a new suite of structure formation and radiative transfer simulations
from the PRACE4LOFAR project designed to investigate whether the mechanism of
radiative feedback, or the suppression of star formation in ionized regions
from UV radiation, can be inferred from these observations. Our source halo
mass extends down to $10^8 M_\odot$, with sources in the mass range $10^8$ to
$10^9 M_\odot$ expected to be particularly susceptible to feedback from
ionizing radiation, and we vary the aggressiveness and nature of this
suppression. Not only do we have four distinct source models, we also include
two box sizes (67 Mpc and 349 Mpc), each with two grid resolutions. This suite
of simulations allows us to investigate the robustness of our results. All of
our simulations are broadly consistent with the observed electron-scattering
optical depth of the cosmic microwave background and the neutral fraction and
photoionization rate of hydrogen at $z\sim6$. In particular, we investigate the
redshifted 21-cm emission in anticipation of upcoming radio interferometer
observations. We find that the overall shape of the 21-cm signal and various
statistics are robust to the exact nature of source suppression, the box size,
and the resolution. There are some promising model discriminators in the
non-Gaussianity and small-scale power spectrum of the 21-cm signal.
