A Deep Search for Extended Radio Continuum Emission From Dwarf Spheroidal Galaxies: Implications for Particle Dark Matter

TL;DR

This study uses deep radio observations of dwarf spheroidal galaxies to search for synchrotron emission from dark matter annihilation, setting new limits on particle properties and demonstrating the complementarity of radio and gamma-ray indirect detection methods.

Contribution

First deep radio mapping of multiple dwarf spheroidal galaxies to constrain dark matter annihilation signals and compare results with gamma-ray observations.

Findings

No significant emission detected in Ursa Major II and Willman 1.

Upper limits on WIMP annihilation cross-section comparable to Fermi-LAT gamma-ray constraints.

Radio observations provide valuable, complementary constraints on dark matter properties.

Abstract

We present deep radio observations of four nearby dwarf spheroidal (dSph) galaxies, designed to detect extended synchrotron emission resulting from weakly interacting massive particle (WIMP) dark matter annihilations in their halos. Models by Colafrancesco et al. (CPU07) predict the existence of angularly large, smoothly distributed radio halos in such systems, that stem from electron and positron annihilation products spiraling in a turbulent magnetic field. We map a total of 40.5 deg^2 around the Draco, Ursa Major II, Coma Berenices, and Willman 1 dSphs with the GBT at 1.4 GHz to detect this annihilation signature, greatly reducing discrete-source confusion using the NVSS catalog. We construct radial surface brightness profiles from each of the subtracted maps, and jackknife the data to quantify the significance of the features therein. At the 10 arcmin resolution of our observations, foregrounds contribute a standard deviation of 1.8 - 5.7 mJy/beam to our high-latitude maps, with the emission in the Draco and Coma dominated by foregrounds. On the other hand, we find no significant emission in the Ursa Major II and Willman 1 fields, and explore the implications of non-detections in these fields for particle dark matter using the fiducial models of CPU07. For a WIMP mass of 100 GeV annihilating into $b\bar{b}$ final states and B = 1 muG, upper limits on the annihilation cross-section for Ursa Major II and Willman I are log<ov,cm^3/s> < -25 for the prefereed set of charged particle propagation parameters adopted by CPU07; this is comparable to that inferred at gamma-ray energies from the two-year Fermi-LAT data. We discuss three avenues for improving the constraints on <ov> presented here, and conclude that deep radio observations of dSphs are highly complementary to indirect WIMP searches at higher energies.