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We present the consistent Î´N formalism for curvatureperturbations in anisotropic cosmological backgrounds. We employ ourÎ´N formalism to calculate the power spectrum, the bispectrumand the trispectrum in models of anisotropic inflation with thebackground gauge fields in Bianchi I universe. Our results coincideexactly with the recent results obtained from in-in formalism. Tosatisfy the observational constraints the anisotropies generated onpower spectrum are kept small but large orientation-dependentnon-Gaussianities can be generated. We study the Suyama-Yamaguchiinequality for the amplitudes of the bispectrum and the trispectrumin the presence of anisotropic shapes.
We present a consistent \delta N formalism for curvature perturbations in anisotropic cosmological backgrounds. We employ our \delta N formalism to calculate the power spectrum, the bispectrum and the trispectrum in models of anisotropic inflation with the background gauge fields in Bianchi I universe. Our results coincide exactly with the recent results obtained from in-in formalism. To satisfy the observational constraints the anisotropies generated on power spectrum are kept small but large orientation-dependent non-Gaussianities can be generated. We study the Suyama-Yamaguchi inequality for the amplitudes of the bispectrum and the trispectrum in the presence of anisotropic shapes.
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