  Understanding the nature of the first stars is key to understanding the early
universe. With new facilities such as JWST we may soon have the first
observations of the earliest stellar populations, but to understand these
observations we require detailed theoretical models. Here we compute a grid of
stellar evolution models using the Geneva code with the aim to improve our
understanding of the evolution of zero-metallicity stars, with particular
interest in how rotation affects surface properties, interior structure, and
metal enrichment. We produce a range of models of initial masses (Mini) from
1.7 Msun to 120 Msun, focusing on massive models of 9 Msun < Mini < 120 Msun.
Our grid includes models with and without rotation, with rotating models having
an initial velocity of 40% of the critical velocity. We find that rotation
strongly impacts the evolution of the first stars, mainly through increased
core size and stronger H-burning shells during core He-burning. Without
radiative mass loss, angular momentum builds at the surface in rotating models,
thus models of initial masses Mini > 60 Msun reach critical rotation on the
main sequence and experience mass loss. We find that rotational mixing strongly
affects metal enrichment, but does not always increase metal production as we
see at higher metallicities. This is because rotation leads to an earlier CNO
boost to the H shell during He-burning, which may hinder metal enrichment
depending on initial mass and rotational velocity. Electronic tables of this
new grid of Population III models are publicly available.
