  A recent article uncovered a surprising dynamical mechanism at work within
the (vacuum) Einstein `flow' that strongly suggests that many closed
3-manifolds that do not admit a locally homogeneous and isotropic metric
\textit{at all} will nevertheless evolve, under Einsteinian evolution, in such
a way as to be \textit{asymptotically} compatible with the observed,
approximate, spatial homogeneity and isotropy of the universe
\cite{Moncrief:2015}. Since this previous article, however, ignored the
potential influence of \textit{dark-energy} and its correspondent accelerated
expansion upon the conclusions drawn, we analyze herein the modifications to
the foregoing argument necessitated by the inclusion of a \textit{positive}
cosmological constant --- the simplest viable model for dark energy.
