Faint polarised sources in the Lockman Hole field at 1.4 GHz

TL;DR

This study investigates faint polarised radio sources in the Lockman Hole at 1.4 GHz, revealing their properties, redshift dependence, and implications for cosmic magnetic field evolution using deep radio polarisation data.

Contribution

First detailed analysis of faint polarised sources in the Lockman Hole, linking polarisation properties with redshift and cosmic magnetic field evolution.

Findings

Detected 150 polarised sources with a mean fractional polarisation of 5.4%.

Found an anti-correlation between fractional polarisation and redshift for strong sources.

Observed a discrepancy in number counts likely due to sample variance.

Abstract

We aim to study the nature of the faint, polarised radio source population whose source composition and redshift dependence contain information about the strength, morphology, and evolution of magnetic fields over cosmic timescales. We use a 15 pointing radio continuum L-band mosaic of the Lockman Hole, observed in full polarisation, generated from archival data of the WSRT. The data were analysed using the RM-Synthesis technique. We achieved a noise of 7 {\mu}Jy/beam in polarised intensity, with a resolution of 15''. Using infrared and optical images and source catalogues, we were able to cross-identify and determine redshifts for one third of our detected polarised sources. We detected 150 polarised sources, most of which are weakly polarised with a mean fractional polarisation of 5.4 %. With a total area of 6.5 deg^2 and a detection threshold of 6.25 {\sigma} we find 23 polarised sources per deg^2. Based on our multi wavelength analysis, we find that our sample consists of AGN only. We find a discrepancy between archival number counts and those present in our data, which we attribute to sample variance. Considering the absolute radio luminosty, to distinguish weak and strong sources, we find a general trend of increased probability to detect weak sources at low redshift and strong sources at high redshift. Further, we find an anti-correlation between fractional polarisation and redshift for our strong sources sample at z{\geq}0.6. A decrease in the fractional polarisation of strong sources with increasing redshift cannot be explained by a constant magnetic field and electron density over cosmic scales, however the changing properties of cluster environments over the cosmic timemay play an important role. Disentangling these two effects requires deeper and wider polarisation observations, and better models of the morphology and strength of cosmic magnetic fields.