E-MILES stellar population models do not include the abundance of individual or alpha elements yet, we are restricted to the base models, which assume that \[M/H\]=\[Fe/H\] at solar metallicity. However, this assumption does not hold at low metallicities because the Milky Way stars used in the computation of the models are themselves alpha-enhanced [see @2010MNRAS.404.1639V]. The consequences of possible offsets resulting from non-solar abundance ratios are discussed further below.

The redshifts of our galaxies are of great interest because they set the distances to the galaxies and their physical parameters, and allow a proper classification of the candidates as UDGs. Without additional spectroscopic or redshift-by-association for our sample, we consider a prior that takes into consideration a few assumptions. galaxies with angular sizes $R_e\gtrsim 5$ have only been associated to environments with distances smaller than 100 Mpc , thus we can assume all UDG candidates are nearby. Moreover, all UDG candidates were selected with a minimum effective radius of $R_e=5.3$, which implies a physical radius of $R_e=2.5$ kpc at the distance of Coma, $100$ Mpc, or a redshift of $z\approx 0.023$. At a distance as low as $200$ Mpc, or $z\approx 0.046$, these UDGs would all already have an effective 