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Modified gravity (MG) theories aim to reproduce the observed acceleration ofthe Universe by reducing the dark sector while simultaneously recoveringGeneral Relativity (GR) within dense environments. Void studies appear to be asuitable scenario to search for imprints of alternative gravity models oncosmological scales. Voids cover an interesting range of density scales wherescreening mechanisms fade out, which reaches from a density contrast $\delta\approx -1$ close to their centers to $\delta \approx 0$ close to theirboundaries. We present an analysis of the level of distinction between GR andtwo modified gravity theories, the Hu-Sawicki $f(R)$ and the symmetron theory.This study relies on the abundance, linear bias, and density profile of voidsdetected in n-body cosmological simulations. We define voids as connectedregions made up of the union of spheres with a {\it \textup{mean}} densitygiven by $\overline\rho_v=0.2\,\overline\rho_m$, but disconnected from anyother voids. We find that the height of void walls is considerably affected bythe gravitational theory, such that it increases for stronger gravitymodifications. Finally, we show that at the level of dark matter n-bodysimulations, our constraints allow us to distinguish between GR and MG modelswith $|f_{R0}| > 10^{-6}$ and $z_{SSB} > 1$. Differences of best-fit values forMG parameters that are derived independently from multiple void probes mayindicate an incorrect MG model. This serves as an important consistency check.

Cosmic voids in modified gravity scenarios