CMB hemispherical asymmetry from non-linear isocurvature perturbations

Abstract

We investigate whether non-adiabatic perturbations from inflation could produce an asymmetric distribution of temperature anisotropies on large angular scales in the cosmic microwave background (CMB). We use a generalised non-linear $\delta N$ formalism to calculate the non-Gaussianity of the primordial density and isocurvature perturbations due to the presence of non-adiabatic, but approximately scale-invariant field fluctuations during multi-field inflation. This local-type non-Gaussianity leads to a correlation between very long wavelength inhomogeneities, larger than our observable horizon, and smaller scale fluctuations in the radiation and matter density. Matter isocurvature perturbations contribute primarily to low CMB multipoles and hence can lead to a hemispherical asymmetry on large angular scales, with negligible asymmetry on smaller scales. In curvaton models, where the matter isocurvature perturbation is partly correlated with the primordial density perturbation, we are unable to obtain a significant asymmetry on large angular scales while respecting current observational constraints on the observed quadrupole. However in the axion model, where the matter isocurvature and primordial density perturbations are uncorrelated, we find it may be possible to obtain a significant asymmetry due to isocurvature modes on large angular scales. Such an isocurvature origin for the hemispherical asymmetry would naturally give rise to a distinctive asymmetry in the CMB polarisation on large scales.

15 pages, 5 figures

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Cited by in corpus (7)

• Pre-inflationary primordial perturbations
• Expected dipole asymmetry in CMB polarization
• Strongly scale-dependent CMB dipolar asymmetry from super-curvature fluctuations
• Finslerian dipolar modulation of the CMB power spectra at scales $2<l<600$
• CMB Polarization by the Asymmetric Template of Scalar Perturbations
• Analytical study of classic models of Hybrid Inflation
• Spectator fields and their imprints on the Cosmic Microwave Background