Radio emission from dark matter annihilation in the Large Magellanic Cloud

Abstract

The Large Magellanic Cloud, at only 50 kpc away from us and known to be dark matter dominated, is clearly an interesting place where to search for dark matter annihilation signals. In this paper, we estimate the synchrotron emission due to WIMP annihilation in the halo of the LMC at two radio frequencies, 1.4 and 4.8 GHz, and compare it to the observed emission, in order to impose constraints in the WIMP mass vs. annihilation cross section plane. We use available Faraday rotation data from background sources to estimate the magnitude of the magnetic field in different regions of the LMC's disc, where we calculate the radio signal due to dark matter annihilation. We account for the e+ e- energy losses due to synchrotron, Inverse Compton Scattering and bremsstrahlung, using the observed hydrogen and dust temperature distribution on the LMC to estimate their efficiency. The extensive use of observations, allied with conservative choices adopted in all the steps of the calculation, allow us to obtain very realistic constraints.

9 pages, 7 figures

References in corpus (8)

• Observation of an anomalous positron abundance in the cosmic radiation
• Dark Matter Candidates from Particle Physics and Methods of Detection
• Measurement of the Cosmic Ray e+ plus e- spectrum from 20 GeV to 1 TeV with the Fermi Large Area Telescope
• Dark matter interpretation of recent electron and positron data
• Detecting dark matter WIMPs in the Draco dwarf: a multi-wavelength perspective
• Radio constraints on dark matter annihilation in the galactic halo and its substructures
• Constraining Supersymmetric Dark Matter With Synchrotron Measurements
• X-ray Radiation from the Annihilation of Dark Matter at the Galactic Center