Quantum Fluctuations of Vector Fields and the Primordial Curvature Perturbation in the Universe

TL;DR

This paper extends the  N formalism to include vector field perturbations, revealing anisotropic particle production and its impact on primordial curvature perturbations, with potential observational signatures of vector field contributions.

Contribution

It introduces a formalism for vector field perturbations in the  N approach, analyzing anisotropic effects and their observational signatures in curvaton and end-of-inflation models.

Findings

Vector particle production is generally anisotropic.

Generated  is statistically anisotropic if parameters p or q are non-zero.

Anisotropic non-linearity parameter fNL correlates with spectral anisotropy.

Abstract

The \delta N formalism is extended to include the perturbation of the vector field. The latter is quantized in de Sitter space-time and it is found that in general the particle production process of the vector field is anisotropic. This anisotropy is parametrized by introducing two parameters p and q, which are determined by the conformal invariance breaking mechanism. If any of them are non-zero, generated \zeta is statistically anisotropic. Then the power spectrum of \zeta and the non-linearity parameter fNL have an angular modulation. This formalism is applied for two vector curvaton models and the end-of-inflation scenario. It is found that for p \ne 0, the magnitude of fNL and the direction of its angular modulation is correlated with the anisotropy in the spectrum. If p \gtrsim 1, the anisotropic part of fNL is dominant over the isotropic one. These are distinct observational signatures; their detection would be a smoking gun for a vector field contribution to \zeta . In the first curvaton model the vector field is non-minimally coupled to gravity and in the second one it has a time varying kinetic function and mass. In the former, only statistically anisotropic \zeta can be generated, while in the latter, isotropic \zeta may be realized too. Parameter spaces for these vector curvaton scenarios are large enough for them to be realized in the particle physics models. In the end-of-inflation scenario fNL have similar properties to the vector curvaton scenario with additional anisotropic term.