Second-order power spectra of CMB anisotropies due to primordial random perturbations in flat cosmological models

Details Second-order power spectra of CMB anisotropies due to primordial random perturbations in flat cosmological models Second-order power spectra of CMB anisotropies due to primordial random perturbations in flat cosmological models

2007-12-15

arxiv.org/abs/0712.2511v3

Phys.Rev.D77:103521,2008

Astronomy and Astrophysics

Astrophysics

11 pages

Scientific paper

10.1103/PhysRevD.77.103521

Second-order power spectra of Cosmic Microwave Background (CMB) anisotropies due to random primordial perturbations at the matter dominant stage are studied, based on the relativistic second-order theory of perturbations in flat cosmological models and on the second-order formula of CMB anisotropies derived by Mollerach and Matarrese. So far the second-order integrated Sachs-Wolfe effect has been analyzed using the three-point correlation or bispectrum. In this paper we derive the second-order term of power spectra given using the two-point correlation of temperature fluctuations. The second-order density perturbations are small, compared with the first-order ones. The second-order power spectra of CMB anisotropies, however, are not small at all, compared with the first-order power spectra, because at the early stage the first-order integrated Sachs-Wolfe effect is very small and the second-order integrated Sachs-Wolfe effect may be dominant over the first-order ones. So their characteristic behaviors may be measured through the future precise observation and bring useful informations on the structure and evolution of our universe in the future.

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