Relationship between parameters used for sample selection (stellar mass M_* [M_⊙], half-light radius in rest-frame g-band r_1∕2 [kpc], and Sérsic index n) with inclination (in the form of 1 − cos(i)). The distributions are shown for galaxies in our parent samples (see Sects. 2.1., 2.2., and 2.3). A histogram of the inclination distribution (or equivalently axis ratio distribution) is shown in the top panels. Galaxies randomly oriented would produce a flat distribution. Dips in the local b∕a distribution are caused by numerical issues in the Simard et al. (2011) fitting. Teal dots trace the median values in bins of inclination and the pink curves show the resulting power-law fit (Eq. (3)) to the medians. We subtract the inclination dependent term from our parameters before performing our final sample selection to avoid artificially introducing inclination trends in our results.