Radio Signal by Galactic Dark Matter

TL;DR

This paper explores how radio emissions caused by electrons and positrons from dark matter annihilation can be used to detect or constrain dark matter properties, focusing on synchrotron radiation in the galactic halo.

Contribution

It proposes a method to constrain WIMP dark matter properties using radio observations of synchrotron radiation from galactic substructures.

Findings

Derived bounds on dark matter annihilation cross-section.

Estimated sensitivity of radio signals to dark matter mass.

Highlighted astrophysical uncertainties affecting constraints.

Abstract

An interesting strategy for indirect detection of Dark Matter comes through the amounts of electrons and positrons usually emitted by DM pair annihilation. The e+e- gyrating in the galactic magnetic field then produce secondary synchrotron radiation. The radio emission from the galactic halo as well as from its expected substructures if compared with the measured diffuse radio background can provide constraints on the physics of WIMPs. In particular one gets the bound of <sigma_A*v> = 10^{-24} cm^3 s^{-1} for a DM mass m_chi = 100 GeV even though sensibly depending on the astrophysical uncertainties.