We study the final collapse of rotating and non-rotating
very massive star progenitors with zero-age-main-sequence
masses of 60, 80, and 115 $\mathrm{M}_\odot$ by 2D hydrodynamics simulations.
The general relativistic radiation hydrodynamics code NADA-FLD allows us to follow the evolution
beyond the moment when the newly born neutron star (NS) collapses to a
black hole (BH), which happens within 350-580 ms after bounce in all cases.
In all cases except the rapidly rotating 60$\mathrm{M}_\odot$ model, neutrino heating leads to shock revival. In the rapidly rotating 60 $\mathrm{M}_\odot$ model, centrifugal
effects support higher NS mass but reduce the radiated neutrino luminosities
and mean energies, and the value of neutrino-heating rate is smaller by roughly a factor of two compared to its non-rotating counterpart. After BH formation, the neutrino luminosities drop steeply but continue
on a 1-2 orders of magnitude lower level for several 100\,ms because of aspherical
accretion of neutrino and shock-heated matter. In all shock-reviving models BH accretion swallows the entire neutrino-heated matter and the explosion energies decrease from maxima to zero within a few seconds latest. Nevertheless, the shock or a sonic pulse moves outward and may trigger mass loss, which we estimate
by long-time simulations with the Prometheus code.