Astrophysical Constraints on Inflationary Dark Matter in the Luminogenesis Model

TL;DR

This paper explores how astrophysical data constrains inflationary dark matter within the luminogenesis model, linking dark matter properties, inflation, and astrophysical observations to refine model parameters.

Contribution

It provides the first constraints on inflationary dark matter in the luminogenesis model, connecting astrophysical phenomena with particle physics and inflationary parameters.

Findings

Upper bound on the symmetry breaking scale of the inflaton

Constraints on the decoupling scale M_1 of gauge group representations

Linking astrophysical data to dark matter and inflation parameters

Abstract

The assumption of collisionless cold dark matter on its own cannot reconcile several astrophysical discrepancies (cusp-vs-core problem, missing satellite problem, too-big-to-fail problem). Self-interacting dark matter provides a promising framework for solving all these problems, and self-interaction cross sections are duly constrained in the literature. Following the work of Tulin, Yu, and Zurek [1], we can constrain the dark matter mass and the mass of a light mediator assuming a generic scalar Yukawa-type interaction. In particular, we constrain the strongly coupled inflationary dark matter of the luminogenesis model, a unification model with the gauge group $SU(3)_C \times SU(6) \times U(1)_Y$, which breaks to the Standard Model with an extra gauge group for dark matter when the inflaton rolls into its true vacuum. The luminogenesis model is additionally subject to constraints on inflation, and we find an upper bound on the scale of symmetry breaking of the inflaton and the decoupling scale $M_1$ of certain representations of the gauge group. We emphasize that the luminogenesis model enables a unique connection between astrophysical constraints, the nature of dark matter, and inflation.