Filaments in and between galaxy clusters at low and mid-frequency with the SKA

Journal Article · Tue Nov 26 00:00:00 EST 2024 · Astronomy and Astrophysics

DOI:https://doi.org/10.1051/0004-6361/202349095· OSTI ID:2564647

Vacca, Valentina ^[1]; Govoni, Federica ^[2]; Murgia, Matteo ^[2]; Loi, Francesca ^[2]; Feretti, Luigina ^[3]; Li, Hui ^[4]; Battistelli, Elia ^[5]; Enßlin, Torsten A. ^[6]; Marchegiani, Paolo ^[2]

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1. Istituto Nazionale di Astrofisica (INAF)-OAC, Selargius (Italy); Max Planck Institute for Astrophysics, Garching (Germany)
2. Istituto Nazionale di Astrofisica (INAF)-OAC, Selargius (Italy)
3. Istituto Nazionale di Astrofisica (INAF), Bologna (Italy)
4. Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
5. Univ. of Rome (Italy)
6. Max Planck Institute for Astrophysics, Garching (Germany)

Context. Understanding the magnetised Universe is a major challenge in modern astrophysics, and cosmic magnetism has been acknowledged as one of the key scientific drivers of the most ambitious radio instrument ever planned, the Square Kilometre Array. Aims. With this work, we aim to investigate the potential of the Square Kilometre Array and its precursors and pathfinders in the study of magnetic fields in galaxy clusters and filaments through diffuse synchrotron radio emission. Galaxy clusters and filaments of the cosmic web are indeed unique laboratories in which to investigate turbulent fluid motions and large-scale magnetic fields in action, and much of what is known about magnetic fields in galaxy clusters comes from sensitive radio observations. Methods. Based on cosmological magneto-hydrodynamic simulations, we predict radio properties (total intensity and polarisation) of a pair of galaxy clusters connected by a cosmic-web filament. Results. We use our theoretical expectations to explore the potential of polarimetric observations to study large-scale structure magnetic fields in the frequency ranges 50–350 MHz and 950–1760 MHz. We also present predictions for galaxy cluster polarimetric observations with the Square Kilometre Array precursors and pathfinders, such as the LOw frequency ARray 2.0 and the MeerKAT+ telescope. Conclusions. Our findings point out that polarisation observations are particularly powerful for the study of large-scale magnetic fields, since they are not significantly affected by confusion noise. The unprecedented sensitivity and spatial resolution of the intermediatefrequency radio telescopes make them the favourite instruments for the study of these sources through polarimetric data, potentially allowing us to understand if the energy density of relativistic electrons is in equipartition with the magnetic field or rather coupled with the thermal gas density. Our results show that low-frequency instruments also represent a precious tool to study diffuse synchrotron emission in total intensity and polarisation.

• Research Organization: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
• Sponsoring Organization: USDOE Laboratory Directed Research and Development (LDRD) Program
• Grant/Contract Number: 89233218CNA000001
• OSTI ID: 2564647
• Report Number(s): LA-UR--25-23601
• Journal Information: Astronomy and Astrophysics, Journal Name: Astronomy and Astrophysics Vol. 691; ISSN 0004-6361
• Publisher: EDP Sciences
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
acceleration of particles
galaxies: clusters: intracluster medium
large-scale structure of Universe
magnetic fields
polarization
radiation mechanisms: non-thermal