Hamiltonian formalism for cosmological perturbations: the separate-universe approach

Abstract

The separate-universe approach provides an effective description of cosmological perturbations at large scales, where the universe can be described by an ensemble of independent, locally homogeneous and isotropic patches. By reducing the phase space to homogeneous and isotropic degrees of freedom, it greatly simplifies the analysis of large-scale fluctuations. It is also a prerequisite for the stochastic-inflation formalism. In this work, we formulate the separate-universe approach in the Hamiltonian formalism, which allows us to analyse the full phase-space structure of the perturbations. Such a phase-space description is indeed required in dynamical regimes which do not benefit from a background attractor, as well as to investigate quantum properties of cosmological perturbations. We find that the separate-universe approach always succeeds in reproducing the same phase-space dynamics for homogeneous and isotropic degrees of freedom as the full cosmological perturbation theory, provided that the wavelength of the modes under consideration are larger than some lower bound that we derive. We also compare the separate-universe approach and cosmological perturbation theory at the level of the gauge-matching procedure, where the agreement is not always guaranteed and requires specific matching prescriptions that we present.

Discussion around equation (4.12) expanded, few minor changes (main conclusions unchanged)

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• Hamiltonian formalism for cosmological perturbations: fixing the gauge
• On the Hamilton-Jacobi approach to inflation beyond slow roll
• Gauge-invariant perturbations at a quantum gravity bounce
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• Stochastic Inflation in Numerical Relativity
• $\delta N$ formalism on the past light-cone
• The validity of separate-universe approach in transient ultra-slow-roll inflation
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• $\delta N$ formalism with gradient interactions
• Dynamically generated tilt of isocurvature fluctuations
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