Neutralino Dark Matter as the Source of the WMAP Haze

TL;DR

This paper explores whether neutralino dark matter within the supersymmetric framework can account for the WMAP Haze, analyzing the parameter space of the CMSSM to identify regions consistent with the observed emission.

Contribution

It demonstrates that most of the CMSSM parameter space predicts neutralinos capable of explaining the WMAP Haze, highlighting specific regions like focus point, A-funnel, and bulk as compatible.

Findings

Neutralino properties in certain CMSSM regions match the WMAP Haze features.

Focus point, A-funnel, and bulk regions predict suitable neutralino masses and annihilation modes.

Stau-coannihilation region is disfavored for explaining the Haze.

Abstract

Previously, it has been argued that the anomalous emission from the region around the Galactic Center observed by WMAP, known as the ``WMAP Haze'', may be the synchrotron emission from relativistic electrons and positrons produced in dark matter annihilations. In particular, the angular distribution, spectrum, and intensity of the observed emission are consistent with the signal expected to result from a WIMP with an electroweak-scale mass and an annihilation cross section near the value predicted for a thermal relic. In this article, we revisit this signal within the context of supersymmetry, and evaluate the parameter space of the Constrained Minimal Supersymmetric Standard Model (CMSSM). We find that, over much of the supersymmetric parameter space, the lightest neutralino is predicted to possess the properties required to generate the WMAP Haze. In particular, the focus point, A-funnel, and bulk regions typically predict a neutralino with a mass, annihilation cross section, and dominant annihilation modes which are within the range required to produce the observed features of the WMAP Haze. The stau-coannihilation region, in contrast, is disfavored as an explanation for the origin of this signal.