Baryonic Tully-Fisher relation comparing the placement of our sample with respect to various samples from the literature. Galaxies in our sample with well constrained rotational velocity (see Appendix C for more details) are denoted as in Fig. 8. We note that the placement on the BTFR is robust for all galaxies (both optically reliable and unreliable) as derived stellar mass is not significantly impacted by the shape of the Sérsic fit (see Sect. 3.3.1 for more details); only the UDG classification of the optically unreliable ones is less certain. For galaxies that show a flattening in the PV slice along the major axis, we provide errors on circular velocities, while others we plot as lower limits. Black dash dotted line is the best fit model to the SPARC sample from Lelli et al. (2016a).