Radio Emission in the Cosmic Web
Pablo A. Araya-Melo, Miguel A. Aragon-Calvo, Marcus Brueggen and, Matthias Hoeft

TL;DR
This study investigates radio emissions in the cosmic web by analyzing shock waves in cosmological simulations, classifying structures, and estimating radio flux, providing insights into the detectability of cosmic web radio signals.
Contribution
It introduces a calibrated shock finding method in SPH simulations and applies the SpineWeb technique to classify cosmic web structures for radio emission analysis.
Findings
Median Mach numbers vary across structures: clusters ~1.8, filaments ~6.2, walls ~7.5, voids ~18.
A shock energy dissipation fraction of 0.0005 matches observational data.
41% of massive clusters host diffuse radio relics, and filament radio flux is predicted at 0.12 μJy at 150 MHz.
Abstract
We explore the possibility of detecting radio emission in the \emph{cosmic web} by analyzing shock waves in the MareNostrum cosmological simulation. This requires a careful calibration of shock finding algorithms in Smoothed-Particle Hydrodynamics simulations, which we present here. Moreover, we identify the elements of the cosmic web, namely voids, walls, filaments and clusters with the use of the SpineWeb technique, a procedure that classifies the structure in terms of its topology. Thus, we are able to study the Mach number distribution as a function of its environment. We find that the median Mach number, for clusters is , for filaments is , for walls is , and for voids is . We then estimate the radio emission in the…
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