Gamma-ray lines and One-Loop Continuum from s-channel Dark Matter Annihilations

TL;DR

This paper investigates conditions under which dark matter models produce enhanced gamma-ray line signals relative to the continuum, focusing on 1-loop annihilation processes in s-channel fermionic dark matter models with vector or scalar mediators.

Contribution

It identifies specific coupling and mass conditions that lead to large gamma-ray line signals in fermionic dark matter models, including detailed 1-loop calculations and model predictions.

Findings

Large line over continuum ratio models are identified.

Conditions for enhanced gamma-ray lines are established.

Predictions are made for current and future gamma-ray telescopes.

Abstract

The era of indirect detection searches for dark matter has begun, with the sensitivities of gamma-ray detectors now approaching the parameter space relevant for weakly interacting massive particles. In particular, gamma ray lines would be smoking gun signatures of dark matter annihilation, although they are typically suppressed compared to the continuum. In this paper, we pay particular attention to the 1-loop continuum generated together with the gamma-ray lines and investigate under which conditions a dark matter model can naturally lead to a line signal that is relatively enhanced. We study generic classes of models in which DM is a fermion that annihilates through an s-channel mediator which is either a vector or scalar and identify the coupling and mass conditions under which large line signals occur. We focus on the "forbidden channel mechanism" advocated a few years ago in the "Higgs in space" scenario for which tree level annihilation is kinematically forbidden today. Detailed calculations of all 1-loop annihilation channels are provided. We single out very simple models with a large line over continuum ratio and present general predictions for a large range of WIMP masses that are relevant not only for Fermi and Hess II but also for the next generation of telescopes such as CTA and Gamma-400. Constraints from the relic abundance, direct detection and collider bounds are also discussed.