  In this Letter, we report the outcomes of 1-D modelling of a rotating 25
M$_{\odot}$ zero-age main-sequence Population III star up to the stage of the
onset of core collapse. Rapidly rotating models display violent and sporadic
mass losses after the Main-Sequence stage. In comparison to the solar
metallicity model, Pop III models show very small pre-supernova radii. Further,
with models at the stage of the onset of core collapse, we simulate the
hydrodynamic simulations of resulting supernovae. Depending upon the mass
losses due to corresponding rotations and stellar winds, the resulting
supernovae span a class from weak Type II to Type Ib/c. We find that the
absolute magnitudes of the core-collapse supernovae resulting from Pop III
stars are much fainter than that resulting from a solar metallicity star. From
our simulation results, we also conclude that within the considered limits of
explosion energies and Nickel masses, these transient events are very faint,
making it difficult for them to be detected at high redshifts.
