  The first stars continue to elude modern telescopes, but much has been
accomplished in observing the glow of the first galaxies. As detection
capabilities improve we will eventually resolve these galaxies, but hopes of
observing an individual star remains dim for the foreseeable future. However,
our first view of an individual first star may be possible due to its
explosion. In this work, we present evolution calculations for Population III
(Pop III) stars and their subsequent supernovae explosions. Our evolution
models include a mass range of 15 - 100 M$_\odot$, each with initial heavy
element abundance Z = 10-14. Our models are evolved from pre-main sequence
through formation of an iron core, and thus near to core collapse. We find that
modelling the evolution of these stars is very sensitive to the choice of
convection criterion; here we provide evolution results using both the
Schwarzschild and Ledoux criteria. We also use the final structure from our
models for numerical simulation of their supernovae light curves using a
radiation hydrodynamics code. In doing so, we estimate a lower bound of initial
model mass that may be possible to observe in the near future. We also find
that our 40 M$_\odot$ Schwarzschild evolution model produces the brightest
supernova peak and statistically should be the most frequently observed. At our
highest redshift z= 15, only the 60 M$_\odot$ Schwarzschild model at peak
magnitude starts to rival the 40 M$_\odot$ model in brightness.
