Curvature fluctuations on asymptotically de Sitter spacetimes via the
  semiclassical Einstein's equations
  It has been proposed recently to consider in the framework of cosmology an
extension of the semiclassical Einstein's equations in which the Einstein
tensor is considered as a random function. This paradigm yields a hierarchy of
equations between the $n$-point functions of the quantum, normal ordered,
stress energy-tensor and those associated to the stochastic Einstein tensor.
Assuming that the matter content is a conformally coupled massive scalar field
on de Sitter spacetime, this framework has been applied to compute the power
spectrum of the quantum fluctuations and to show that it is almost
scale-invariant. We test the robustness and the range of applicability of this
proposal by applying it to a less idealized, but physically motivated,
scenario, namely we consider Friedmann-Robertson-Walker spacetimes which behave
only asymptotically in the past as a de Sitter spacetime. We show in particular
that, under this new assumption and independently from any renormalization
freedom, the power spectrum associated to scalar perturbations of the metric
behaves consistently with an almost scale-invariant power spectrum.
