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CMB Anisotropies at Second Order I
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We present the computation of the full system of Boltzmann equations at second-order describing the evolution of the photon, baryon and cold dark matter fluids. These equations allow to follow the time evolution of the Cosmic Microwave Background (CMB) anisotropies at second-order at all angular scales from the early epoch, when the cosmological perturbations were generated, to the present through the recombination era. This paper sets the stage for the computation of the full second-order radiation transfer function at all scales and for a a generic set of initial conditions specifying the level of primordial non-Gaussianity. In a companion paper, we will present the computation of the three-point correlation function at recombination which is so relevant for the issue of non-Gaussianity in the CMB anisotropies.
Forward citations
Cited by 2 Pith papers
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The Fate of Large Scale White Noise in Second-Order Cosmological Perturbation Theory
White noise in the second-order kurvature density is real, but it is not inherited by the comoving curvature perturbation as an infrared pole, invalidating the k_BH bound on the small-scale primordial power spectrum.
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Anisotropies and non-Gaussianity of the Cosmological Gravitational Wave Background
The angular anisotropy and bispectrum of the cosmological gravitational wave background can encode primordial perturbations, including order-one frequency dependence and primordial non-Gaussianity.
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