Speaker
Description
The MWA is a low-frequency radio telescope that can probe galaxy clusters on Mega-parsec scales via their non-thermal, diffuse synchrotron emission. Using the Galactic and Extragalactic All-sky MWA (GLEAM) survey (Wayth et al. 2015, Hurley-Walker et al. 2017), we have identified over 500 candidate sources of such emission, increasing from the known ~ 100 examples. These sources, halos and relics, are thought to be formed through shocks and turbulence in the intra-cluster medium, tracing large-scale structure formation and the magnetic fields permeating the clusters. With the upgrade of the MWA to Phase II, the increase in maximum baseline has resulted in almost double the available resolution. We have been leveraging this increase in resolution to re-observe a selection of our original candidates. We will present our data-processing pipeline, the challenges involved with MWA Phase II data processing, the results from our sample to date, and show that the MWA in its extended configuration is able to better determine the nature of these sources.
| Suggested presentation duration (minutes) | 15-20 |
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