Radio Emission in the Cosmic Web

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 ${\mathcal{M}}_{\mathrm{clusters}}\approx 1.8$, for filaments is ${\mathcal{M}}_{\mathrm{filaments}}\approx 6.2$, for walls is ${\mathcal{M}}_{\mathrm{walls}}\approx 7.5$, and for voids is ${\mathcal{M}}_{\mathrm{voids}}\approx 18$. We then estimate the radio emission in the cosmic web using the formalism derived in Hoeft & Brüggen (2007). We also find that in order to match our simulations with observational data (e.g., NVSS radio relic luminosity function), a fraction of energy dissipated at the shock of ${\xi }_{\mathrm{e}}=0.0005$ is needed, in contrast with the ${\xi }_{\mathrm{e}}=0.005$ proposed by Hoeft et al. (2008). We find that 41% of clusters with $M\ge 10^{14}{M}_{\odot }$ host diffuse radio emission in the form of radio relics. Moreover, we predict that the radio flux from filaments should be $S_{150MHz}\sim 0.12$ $\mu$Jy at a frequency of 150 MHz.

19 pages, 17 figures, accepted for publication in MNRAS. Minor changes to tex file

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