Rest-frame UV emission line ratios of the MUSE He II λ1640 sample computed with different dust laws. The panels are similar to Fig. 6, but the Gutkin et al. (2016) models are removed for clarity. Only the galaxies with S/N ≥ 2.5 for emission line considered in each panel are shown in the figure. Observed emission line ratios are shown by stars. f = 1 and f = 2 resemble dust corrections that are applied considering no additional attenuation and twice the additional attenuation for ionised gas regions (computed using the Cardelli et al. 1989 attenuation law) compared to stars (computed using the Calzetti et al. 2000 attenuation law). We further show the distribution of the line ratios using the Cardelli et al. (1989), Calzetti et al. (2000), and Reddy et al. (2015, 2016a) attenuation laws.