Abstract
I report on recent work on perturbations of Robertson-Walker spacetimes using the Bardeen-Stewart variables to describe metric perturbations. The gauge freedom available in the formalism is larger than that arising purely from spacetime diffeomorphisms. The associated non-uniqueness and non-locality problems have a simple solution, but the extra gauge freedom must be taken into account to obtain deterministic linearized field equations. The linearized Einstein equation decouples into scalar, vector and tensor sectors; I write down and comment on the equations one obtains using as matter an isentropic perfect fluid.
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