Statistical Techniques for Detecting the Intergalactic Magnetic Field from Large Samples of Extragalactic Faraday Rotation Data

TL;DR

This paper explores statistical methods to detect the intergalactic magnetic field using large-scale extragalactic Faraday rotation data, highlighting the potential of future surveys like SKA to observe filamentary magnetic structures.

Contribution

It proposes a high-pass filtering technique to isolate intergalactic magnetic field signals from Galactic and source contributions in upcoming radio polarization surveys.

Findings

High-pass filter effectively reduces Galactic RM contributions.

Current data insufficient for filament RM estimation.

Future surveys like SKA can detect IGMF structures at 0.1 degree scales.

Abstract

Rotation measure (RM) grids of extragalactic radio sources have been widely used for studying cosmic magnetism. But their potential for exploring the intergalactic magnetic field (IGMF) in filaments of galaxies is unclear, since other Faraday-rotation media such as the radio source itself, intervening galaxies, and the interstellar medium of our Galaxy are all significant contributors. We study statistical techniques for discriminating the Faraday rotation of filaments from other sources of Faraday rotation in future large-scale surveys of radio polarization. We consider a 30 degree times 30 degree field-of-view toward the south Galactic pole, while varying the number of sources detected in both present and future observations. We select sources located at high redshifts and toward which depolarization and optical absorption systems are not observed, so as to reduce the RM contributions from the sources and intervening galaxies. It is found that a high-pass filter can satisfactorily reduce the RM contribution from the Galaxy, since the angular scale of this component toward high Galactic latitudes would be much larger than that expected for the IGMF. Present observations do not yet provide a sufficient source density to be able to estimate the RM of filaments. However, from the proposed approach with forthcoming surveys, we predict significant residuals of RM that should be ascribable to filaments. The predicted structure of the IGMF down to scales of 0.1 degree should be observable with data from the SKA, if we achieve selections of sources toward which sight lines do not contain intervening galaxies and RM errors are less than a few rad m-2.