Empirical models often rely on key relations from the galaxy--halo connection to construct mock galaxy catalogues. These relations typically describe central galaxies (i. e. the main galaxy of a halo) more accurately than satellite galaxies, which are generally less massive and orbit within larger haloes. Satellite galaxies are affected by a variety of physical processes that pose significant challenges for modelling. In this work, we used v_̊m max. We additionally provide an analytical model for the evolution of these properties. We then examine the evolution of the satellite mass profiles. We find that, although stripping is strongest in the outer regions, the intermediate and inner parts of the satellites experience mass loss at early times. The results of this work can be used by empirical models and galaxy formation models built on gravity-only simulations to improve their descriptions of satellite galaxies. a state-of-the-art cosmological hydrodynamic simulation, to study the evolution of the baryonic component of satellite galaxies. Using the merger trees from this simulation, we followed the evolution of all z=0 satellite galaxies, tracking their stellar mass, gas mass, and r- and U-band magnitudes. We characterised this evolution using proxies including the fraction of subhalo mass and the remaining maximum circular velocity relative to infall, the pericentric distance, and the time since infall. All of these quantities are commonly available in gravity-only simulations and can therefore be used to model these trends in simpler galaxy population models. We find that the gas mass, which is well described by the remaining subhalo mass fraction, declines much more rapidly than the other components, with satellites losing ∼ 80% of their gas by the time the subhalo has lost half of its total mass. By contrast, the evolution of stellar mass and magnitudes is slower overall and is better described by the reduction of the satellite subhalo maximum circular velocity
Contreras et al. (Wed,) studied this question.