  Fallback in core-collapse supernovae is considered a major ingredient for
explaining abundance anomalies in metal-poor stars and the natal kicks and
spins of black holes (BHs). We present a first 3D simulation of BH formation
and fallback in an "aborted" neutrino-driven explosion of a $40$ solar mass
zero-metallicity progenitor from collapse to shock breakout. We follow the
phase up to BH formation using the relativistic CoCoNuT-FMT code. For the
subsequent evolution to shock breakout we apply the moving-mesh code Arepo to
core-collapse supernovae for the first time. Our simulation shows that despite
early BH formation, neutrino-heated bubbles can survive for tens of seconds
before being accreted, leaving them sufficient time to transfer part of their
energy to sustain the shock wave as is propagates through the envelope.
Although the initial net energy ($\sim 2$ Bethe) of the neutrino-heated ejecta
barely equals the binding energy of the envelope, $11\,\mathrm{M}_\odot$ of
hydrogen are still expelled with an energy of $0.23$ Bethe. We find no
significant mixing and only a modest BH kick and spin, but speculate that
stronger effects could occur for slightly more energetic explosions or
progenitors with less tightly bound envelopes.
