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Quantifying the connection between galaxies and their host dark matter haloshas been key for testing cosmological models on various scales. Below $M_\star\sim 10^9\,M_\odot$, such studies have primarily relied on the satellite galaxypopulation orbiting the Milky Way. Here we present new constraints on theconnection between satellite galaxies and their host dark matter subhalos usingthe largest sample of satellite galaxies in the Local Volume ($D \lesssim12\,\mathrm{Mpc}$) to date. We use $250$ confirmed and $71$ candidate dwarfsatellites around 27 Milky Way (MW)-like hosts from the Exploration of LocalVolumE Satellites (ELVES) Survey and use the semi-analytical SatGen model forpredicting the population of dark matter subhalos expected in the same volume.Through a Bayesian model comparison of the observed and the forward-modeledsatellite stellar mass functions (SSMF), we infer the satellite stellar-to-halomass relation. We find that the observed SSMF is best reproduced when subhalosat the low mass end are populated by a relation of the form $M_\star \proptoM^\alpha_\mathrm{peak}$, with a moderate slope of $\alpha_\mathrm{const}=2.10\pm 0.01$ and a low scatter, constant as a function of the peak halo mass, of$\sigma_\mathrm{const}=0.06^{+0.07}_{-0.05}$. A model with a steeper slope($\alpha_\mathrm{grow}=2.39 \pm 0.06$) and a scatter that grows with decreasing$M_\mathrm{peak}$ is also consistent with the observed SSMF but is notrequired. Our new model for the satellite-subhalo connection, based on hundredsof Local Volume satellite galaxies, is in line with what was previously derivedusing only the Milky Way satellites.

ELVES IV: The Satellite Stellar-to-Halo Mass Relation Beyond the Milky-Way