In this paper it is shown how to obtain, without ever using the background classical equations of motion, a simple second order Hamiltonian involving the Mukhanov-Sasaki variable describing quantum linear scalar perturbations for the case of scalar fields with arbitrary potentials and arbitrary spacelike hypersurfaces. It is a generalization of previous works, where the scalar field potential was absent and the spacelike hypersurfaces were flat. This was possible due to the implementation of a new method, together with the Faddeev-Jackiw procedure for the constraint reduction. The resulting Hamiltonian can then be used to study the evolution of quantum cosmological perturbations in quantum backgrounds.

• Received 29 March 2013

DOI:https://doi.org/10.1103/PhysRevD.87.103514