“School of Astronomy”
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| Paper IPM / Astronomy / 13041 |
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We present the consistent δN formalism for curvatureperturbations in anisotropic cosmological backgrounds. We employ ourδN 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 N formalism for curvature perturbations in anisotropic cosmological backgrounds. We employ our 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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