The paper investigates the potential of future dwarf galaxy surveys to constrain galaxy formation and dark matter (DM) physics. Using Milky Way-mass cosmological zoom-in simulations and an empirical galaxy-halo connection model, the authors assess the sensitivity of satellite galaxy populations to galaxy formation cutoffs, warm DM models, and subhalo mass function (SHMF) constraints. They find that observations of all satellites around one MW-mass host can constrain a galaxy formation cutoff at peak virial masses of \(10^8 M_{\odot}\) at the 1σ level but not at the 2σ level due to a tail toward lower masses. Combining hosts with different satellite abundances significantly reduces uncertainties on the cutoff mass scale at the 1σ level but maintains the 2σ tail. The same data can constrain warm DM models with masses of approximately 10-20 keV. SHMF suppression can be constrained to about 70%, 60%, and 50% of the CDM value at peak virial masses of \(10^8\), \(10^9\), and \(10^{10} M_{\odot}\), respectively, while SHMF enhancement constraints are weaker. These results highlight the importance of future surveys like Euclid, the Vera C. Rubin Observatory, and the Nancy Grace Roman Space Telescope in probing new galaxy formation and DM physics.The paper investigates the potential of future dwarf galaxy surveys to constrain galaxy formation and dark matter (DM) physics. Using Milky Way-mass cosmological zoom-in simulations and an empirical galaxy-halo connection model, the authors assess the sensitivity of satellite galaxy populations to galaxy formation cutoffs, warm DM models, and subhalo mass function (SHMF) constraints. They find that observations of all satellites around one MW-mass host can constrain a galaxy formation cutoff at peak virial masses of \(10^8 M_{\odot}\) at the 1σ level but not at the 2σ level due to a tail toward lower masses. Combining hosts with different satellite abundances significantly reduces uncertainties on the cutoff mass scale at the 1σ level but maintains the 2σ tail. The same data can constrain warm DM models with masses of approximately 10-20 keV. SHMF suppression can be constrained to about 70%, 60%, and 50% of the CDM value at peak virial masses of \(10^8\), \(10^9\), and \(10^{10} M_{\odot}\), respectively, while SHMF enhancement constraints are weaker. These results highlight the importance of future surveys like Euclid, the Vera C. Rubin Observatory, and the Nancy Grace Roman Space Telescope in probing new galaxy formation and DM physics.