Distribution of X-ray and radio flux for all simulated pixels in our sky model (Fig. 2). The contours are equally spaced in logarithmic space (Δlog₁₀ = 0.5) and show the distributions of pixels associated with filaments (green), cluster outskirts (blue), or the virial region of galaxy clusters and groups (red). The additional grey lines delimit the regions that will become observable with future X-ray and radio telescopes.