For a sample of S⁴G galaxies, we compare the bar maximum normalized m = 2 Fourier amplitude (upper panel) as measured over 3.6 μm and ICA-corrected maps. Likewise, stellar velocities and inner slopes obtained from 3.6 μm (M/L = 0.53 from E2012) and mass maps (M/L = 0.6 from Meidt et al. 2014) are compared (central and lower panels). Error bars are computed based on boundary disk thicknesses, but the uncertainties coming from the M/L are indeed larger. A lower mass-to-light ratio at 3.6 μm, M/L = 0.47 (McGaugh & Schombert 2014; Querejeta et al. 2015), is also tested for the comparison of maximum velocities of the stellar component of the rotation curve (green empty circles in the central panel). The result from the statistical tests and the number of galaxies in the different subsamples are indicated in Table C.1. When the uncertainty in d_RV_{3.6 μm}(0) associated with the disk thickness is larger than 75 km s^-1 kpc^-1 (upper limit arbitrarily chosen), we exclude the galaxies from the statistics presented in this section.