Measurements of the Cosmological Evolution of Magnetic Fields with the Square Kilometre Array

TL;DR

This paper explores how the Square Kilometre Array can measure and analyze the evolution of magnetic fields in galaxy clusters through Faraday rotation, providing detailed insights into magnetic structures across cosmic time.

Contribution

It demonstrates the SKA's capability to measure magnetic fields in galaxy clusters at various redshifts and proposes methods for detailed magnetic field structure analysis.

Findings

Approximately 10% of the sky is covered by significant extragalactic Faraday screens.

SKA can measure rotation measures up to 5000 rad/m/m in cluster centers.

Full SKA can constrain magnetic field evolution with high precision.

Abstract

We investigate the potential of the Square Kilometre Array (SKA) for measuring the magnetic fields in clusters of galaxies via Faraday rotation of background polarised sources. [...] We find that about 10 per cent of the sky is covered by a significant extragalactic Faraday screen. Most of it has rotation measures between 10 and 100 rad/m/m. We argue that the cluster centres should have up to about 5000 rad/m/m. We show that the proposed mid frequency aperture array of the SKA as well as the lowest band of the SKA dish array are well suited to make measurements for most of these rotation measure values, typically requiring a signal-to-noise of ten. We calculate the spacing of sources forming a grid for the purpose of measuring foreground rotation measures: it reaches a spacing of 36 arcsec for a 100 hour SKA observation per field. We also calculate the statistics for background RM measurements in clusters of galaxies. We find that a first phase of the SKA would allow us to take stacking experiments out to high redshifts (>1), and provide improved magnetic field structure measurements for individual nearby clusters. The full SKA aperture array would be able to make very detailed magnetic field structure measurements of clusters with more than 100 background sources per cluster up to a redshift of 0.5 and more than 1000 background sources per cluster for nearby clusters, and could for reasonable assumptions about future measurements of electron densities in high redshift clusters constrain the power law index for the magnetic field evolution to better than dm=0.4, if the magnetic field in clusters should follow B ~ (1+z)^m.