ApPolLO: Apertif counterparts of Polarised LOFAR sources
Abstract
Knowledge of the structure and evolution of cosmic magnetic fields is indispensable to understand how primordial magnetic fields were generated and amplified during the lifetime of the Universe. Polarisation studies over significant redshift ranges are an important tool in understanding cosmic magnetic fields. We aim to understand the structure and evolution of cosmic magnetic fields, utilising the polarised spectra and depolarisation characteristics of (background) radio sources. Using radio polarisation data at two different frequencies from the LOFAR Rotation Measure (RM) grid catalogue at 144\,MHz and new Apertif data at 1.4\,GHz, we investigate the source statistics of a common sample of polarised sources, deriving the depolarisation ratio between these two frequencies. We utilise this to disentangle depolarising effects local to the source from those along the line of sight. We compile a catalogue of 598 polarised radio components, most of which are located in low-density environments. Fractional polarisation decrease for both wavelengths with redshift. We attributed the main depolarisation at 1.4\,GHz to effects occurring close to the sources, while the depolarisation measured at 144\,MHz is most likely generated by cosmic filaments along the line-of-sight. We were able to get a first redshift dependent upper limit estimate of the RM dispersion in cosmic web filaments.
Related
- LOFAR follow-up of sources in the First LHAASO Catalogue
- Persistent Radio Sources and Multiwavelength Counterparts of Fast Radio Bursts: Magnetar Wind Nebulae and Bow Shocks in Massive Binary Systems
- The Chandra-Gaia Catalog of Counterparts: Resolving ambiguous Gaia matches to X-ray sources in the Chandra Source Catalog using Machine Learning
- HI rotation curves and mass-size relation for 568 galaxies from the Apertif Wide-area Extragalactic Survey
- The MIni-Halos in MIni-Clusters (MIMIC) project. New insights into the origin of mini-halos from a LOFAR, uGMRT, and MeerKAT study of diffuse radio emission in Abell 496 and ZwCl 235
BibTeX
@misc{berger2026appollo,
title = {{ApPolLO: Apertif counterparts of Polarised LOFAR sources}},
author = {A. Berger and B. Adebahr and H. Dénes and R. -J. Dettmar},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.08396},
eprint = {2610.08396},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.08396},
note = {CC BY-NC-ND 4.0},
}
RIS
TY - UNPB
TI - ApPolLO: Apertif counterparts of Polarised LOFAR sources
AU - A. Berger
AU - B. Adebahr
AU - H. Dénes
AU - R. -J. Dettmar
PY - 2026
DA - 2026/10/06
PB - arXiv
DO - 10.48550/arxiv.2610.08396
UR - https://arxiv.org/abs/2610.08396
AB - Knowledge of the structure and evolution of cosmic magnetic fields is indispensable to understand how primordial magnetic fields were generated and amplified during the lifetime of the Universe. Polarisation studies over significant redshift ranges are an important tool in understanding cosmic magnetic fields. We aim to understand the structure and evolution of cosmic magnetic fields, utilising the polarised spectra and depolarisation characteristics of (background) radio sources. Using radio polarisation data at two different frequencies from the LOFAR Rotation Measure (RM) grid catalogue at 144\,MHz and new Apertif data at 1.4\,GHz, we investigate the source statistics of a common sample of polarised sources, deriving the depolarisation ratio between these two frequencies. We utilise this to disentangle depolarising effects local to the source from those along the line of sight. We compile a catalogue of 598 polarised radio components, most of which are located in low-density environments. Fractional polarisation decrease for both wavelengths with redshift. We attributed the main depolarisation at 1.4\,GHz to effects occurring close to the sources, while the depolarisation measured at 144\,MHz is most likely generated by cosmic filaments along the line-of-sight. We were able to get a first redshift dependent upper limit estimate of the RM dispersion in cosmic web filaments.
ER -