  We carry out numerical simulations of the gravitational collapse of a
rotating perfect fluid with the ultrarelativistic equation of state
$P=\kappa\rho$, in axisymmetry in $2+1$ spacetime dimensions with $\Lambda<0$.
We show that for $\kappa \lesssim 0.42$, the critical phenomena are type I and
the critical solution is stationary. The picture for $\kappa \gtrsim 0.43$ is
more delicate: for small angular momenta, we find type II phenomena and the
critical solution is quasistationary, contracting adiabatically. The
spin-to-mass ratio of the critical solution increases as it contracts, and
hence so does that of the black hole created at the end as we fine-tune to the
black-hole threshold. Forming extremal black holes is avoided because the
contraction of the critical solution smoothly ends as extremality is
approached.
