  The first stars might have been fast rotators. This would have important
consequences for their radiative, mechanical and chemical feedback. We discuss
the impact of fast initial rotation on the evolution of massive Population III
models and on their nitrogen and oxygen stellar yields. We explore the
evolution of Population III stars with initial masses in the range of 9Msol <
Mini < 120Msol starting with an initial rotation on the Zero Age Main Sequence
equal to 70% of the critical one. We find that with the physics of rotation
considered here, our rapidly-rotating Population III stellar models do not
follow a homogeneous evolution. They lose very little mass in case mechanical
winds are switched on when the surface rotation becomes equal or larger than
the critical velocity. Impact on the ionising flux appears modest when compared
to moderately-rotating models. Fast rotation favours, in models with initial
masses above ~20Msol, the appearance of a very extended intermediate convective
zone around the H-burning shell during the core He-burning phase. This shell
has important consequences on the sizes of the He- and CO-cores and thus
impacts the final fate of stars. Moreover, it has a strong impact on
nucleosynthesis boosting the production of primary 14N. Fast initial rotation
impacts significantly the chemical feedback of Population III stars.
Observations of extremely metal-poor stars and/or starbursting regions are
essential to provide constraints on the properties of the first stars.
