Notes. In the selection of these samples, we required three conditions. First, the galaxy’s axis ratio is required to be < 0.3 to limit the effect of the galaxy’s inclination on our mass estimates (see Sect. 4). Second, the galaxies should be entirely within the footprints of the surveys or data used. Third, we required the absence of overlapping or nearby bright stars around the galaxy of interest. The 3σ depths of the data were estimated over 10 × 10 arcsec² areas. The uncertainty in these values is ∼1%. All data used are well within the limit needed to detect edges, typically found at μ_g ∼ 26 − 27 mag/arcsec². We also point out that the imaging quality, defined as the full width half maximum (FWHM) of the measured point spread function (PSF), of the different surveys used are very similar (∼1″). At the median distance of the total sample studied here (∼34 Mpc), the smallest structures resolvable with our compiled imaging dataset are of ∼165 pc. Therefore, the compiled dataset is suitable for this study based on both depth and spatial resolution. (1) Venhola et al. (2018), Su et al. (2021), (2) Geha et al. (2017), Mao et al. (2021), (3) Carlsten et al. (2021), Carlsten et al. (2022), (4) Karachentsev et al. (2013), and (5) compiled from Fliri & Trujillo (2016), Román & Trujillo (2018), Nair & Abraham (2010), Maraston et al. (2013).