work, but are still taken into consideration in the analysis of the stellar populations parameters and the redshift.

The metallicity clearly departs from the prior distribution in most cases, with median metallicities systematically small (\[Fe/H\]$\approx -1$ dex). Even though the $1\sigma$ uncertainties remain similar to the prior for the faint UDGs, the posterior distributions for the metallicity are usually skewed towards low metallicities in most cases, and are not flat-shaped like the priors. The main concern in the derived metallicities occur for the more metal-poor galaxies, given that they are sometimes compatible with the lowest metallicity available in our SSP grid (\[Fe/H\]=$-$1.79). Without a larger grid of models, we can not rule out that some of these systems have even lower metallicities. Overall, however, we conclude that our metallicities estimates are well constrained by our SED fitting.

Similarly, despite the large uncertainties for the faint UDGs, we do find that the luminosity-weighted ages tend to be smaller than the prior median (Age $\approx 7$ Gyr). One important point in the evaluation of the ages is that we can see more variation in the SED’s of younger galaxies, in the sense that it is easier to differentiate between a 1 Gyr 