present our arguments why this gives representative results for the warm ionized gas overall. H$\alpha$ is bright enough to allow for independent fits, but is too broad and heavily blended with \[NII\]$\lambda\lambda$6548,6583 in most galaxies to provide good kinematic constraints. Other lines, including H$\beta$, are too faint to be well mapped over large radii. Generally speaking, single-component Gaussians were sufficient to obtain good fits. Exceptions are mentioned in the individual target descriptions in Appendix A.

To monitor the goodness-of-fit and evaluate the need for multiple emission-line components, we also constructed maps of the reduced $\chi^2$, as well as cubes of the fit residuals. Fit residuals are usually below a few percent of the fitted line flux, and median reduced $\chi^2$ are between 0.7 and 5, depending on the degree of contamination with night-sky lines to the emission lines. A notable exception is USS 0211$-$122, which we will further discuss below in §\[ssec:induss0211\].

Our galaxies are too faint in the continuum to study their spectral energy distribution, however, we were able to localize the peak of the continuum emission in 23 targets. We constructed line-free continuum images by averaging along the spectral direction of our data cubes after masking the brightest 