Hess representation of un-convolved and convolved versions of CMD of the simulated dwarf galaxy DG-5. The magnitudes in panel a are a direct result from interpolating on the best matching isochrones (based on the age, metallicity, and mass of the sampled stars). The magnitudes in panel b are obtained by simulating observational errors using the crowding tables used in Meschin et al. (2014) to mimic the quality of real observational data. The color bars indicate the number density of stars in the corresponding plots, and the sparse black points represent individual stars in the CMD.