Ceres is a volatile-rich dwarf planet located in the asteroid belt. Ceres' water-rich nature evidenced itself in low density and telescopic discoveries of a water exosphere (e.g., A'Hearn & Feldman, 1992;McCord et al., 2005). When Dawn reached Ceres in 2015, visible images gathered from the mission revealed a heavily cratered surface with globally uniform albedo with the exception of a few anomalously bright features (e.g., Li et al., 2016). The bright features have been interpreted to represent exposed water ice (e.g., Combe et al., 2016Combe et al., , 2019Landis et al., 2019) which may contribute to Ceres' water exosphere (e.g., Landis et al., 2017). Dawn Gamma Ray and Neutron Detector (GRaND) neutron spectra showed a gradient of H from equator to poles consistent with a gradient of near-surface water ice (Prettyman et al., 2017) and models of thermal stability of ice with depth (Hayne & Aharonson, 2015). Geomorphology similarly suggests the presence of ground ice (e.g., Schmidt et al., 2017). At topographic lows near Ceres' poles, extensive exposed water ice deposits are preserved from sublimation in persistently shadowed regions (e.g., Platz, Nathues, Schorghofer, et al., 2016;Schorghofer et al., 2016).Impact gardening, or the process by which small impacts churn the uppermost surface has been shown to occur on Earth's Moon, through analysis of the depth-distribution of surface-correlated space weathering and radionuclide products observed in the Apollo cores (e.g., Morris, 1978), and must also be occurring on Ceres' surface. Impact gardening will have an effect on the development of Ceres' regolith and, if it is aggressive enough to compete with thermal gradients and sublimation, on the depth to ice. We use published crater size frequency distributions and an updated and generalized impact gardening model to calculate the depth of impact gardening as a function of time on Ceres. The model has been demonstrated to reproduce the gardening observed in Apollo cores returned from the Moon (Costello et al., 2018) and has recently been used to address the evolution of polar ice deposits on the Moon and Mercury (Costello et al., 2020). In this work, we bring the updated gardening and secondary crater production models to bear on the gardening story unfolding on the icy and rocky surface of Ceres.