  Standard quantum theory admits naturally statistical ensembles that are both
pre-selected and post-selected, i.e., they involve both an initial and a final
state. We argue that there is no compelling physical reason to preclude a
probability assignment with a final quantum state at the cosmological level. We
therefore analyze the implications of a final state in the probability
assignment for quantum cosmology. To this end, we derive effective classical
equations of motion for systems subject to both initial and final conditions.
Remarkably, these effective equations do not depend on the details of the
quantum theory, but only on the geometric features of the classical state
space. When applied to Friedman-Robertson-Walker cosmological models, these
effective equations generically describe cosmic acceleration in the absence of
a cosmological constant, dark energy, or modified gravitational dynamics.
Therefore, cosmic acceleration emerges as a quantum post-selection effect, that
is, a macroscopic quantum phenomenon.
