Evaluating the inclination dependence of dust-corrected SFR_FUV values. From top to bottom, the panels show the observed UV SFR, the SFR corrected based on the UV-slope, the hybrid MIR+UV determined SFR, and the SFR corrected based on the Tuffs et al. (2004) radiative transfer models as a function of inclination angle. Face-on galaxies are lie to the left, 1 − cos(i) ~ 0, and edge-on galaxies lie to the right, 1 − cos(i) ~ 1. The blue lines show the inclination relation for SFR_FUV as observed with no dust corrections (top panel). The dust correction factors work to increase the SFR_FUV and lessen the inclination dependence of the SFR. Fitted parameters are given in Table 1. Orange data points show the “restricted sample”, and the full sample is shown as a 2D density histogram. Magenta lines show 150 random realisations of linear parameters from our MCMC chain. Distributions of the y-axes, log(SFR_FUV/SFR_MS) are also displayed as histograms. The dotted line shows where the SFR_FUV = SFR_MS.