with the photometric properties measured in the deeper SMUDGes images. We adopt two different approaches. First, we use the SED fitting photometric redshift to estimate the distance and the total apparent $r$-band magnitude from SMUDGes to determine the total magnitude, assuming a Hubble-Lemaître law with $H_0=70\pm2$ km s$^{-1}$ Mpc$^{-1}$. Next, we use the $r$-band mass-to-light ratio from the E-MILES models [@2010MNRAS.404.1639V; @2012MNRAS.424..172R] to obtain the total stellar mass, assuming that $M_{\odot,r}=4.65$ [@2018ApJS..236...47W]. These calculations are performed using the Monte Carlo chains, and thus the uncertainties are marginalized over all parameters in the SED fitting model. Second, we estimate the stellar mass using the color-mass relation from @2011MNRAS.418.1587T, which is based on data from the survey . Reassuringly, the stellar masses resulting from the two approaches always agree to within $0.1$ dex, which is a difference that is much smaller than the typical mass uncertainties ($\sim$0.8 dex). We conclude that our stellar mass estimates are likely to be dominated by internal random uncertainties rather than by a systematic error in the conversion between luminosity and stellar mass. For the remainder of this work, we use the stellar masses determined using the first method. The stellar masses derived by the first method 