Non-Gaussianity in the Cosmic Microwave Background Induced by Dipolar Dark Matter

TL;DR

This paper explores how dipolar dark matter (DDM) introduces a unique, time-increasing non-Gaussian signature in the cosmic microwave background and large-scale structure, differing from standard cold dark matter predictions.

Contribution

The study extends the DDM model to second order in perturbation theory, revealing a new non-Gaussianity feature that grows over time, unlike typical primordial non-Gaussianities.

Findings

DDM modifies curvature perturbation with a quadratic dipole term

Induces a non-Gaussian bispectrum in the CMB

Non-Gaussianity increases after radiation-matter equality

Abstract

In previous work [L. Blanchet and A. Le Tiec, Phys. Rev. D 80, 023524 (2009)], motivated by the phenomenology of dark matter at galactic scales, a model of dipolar dark matter (DDM) was introduced. At linear order in cosmological perturbations, the dynamics of the DDM was shown to be identical to that of standard cold dark matter (CDM). In this paper, the DDM model is investigated at second order in cosmological perturbation theory. We find that the internal energy of the DDM fluid modifies the curvature perturbation generated by CDM with a term quadratic in the dipole field. This correction induces a new type of non-Gaussianity in the bispectrum of the curvature perturbation with respect to standard CDM. Leaving unspecified the primordial amplitude of the dipole field, which could in principle be determined by a more fundamental description of DDM, we find that, in contrast with usual models of primordial non-Gaussianities, the non-Gaussianity induced by DDM increases with time after the radiation-matter equality on super-Hubble scales. This distinctive feature of the DDM model, as compared with standard CDM, could thus provide a specific signature in the CMB and large-scale structure probes of non-Gaussianity.