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tokens: with increasing radius). However, since we have high-resolution HST imaging for all our galaxies, we prefer to relax this assumption and provide a 2D SFR map. Unlike the emission-line ratios , the modelled emission-line luminosities do have an azimuthal dependence. We assume that the distribution of stellar light in the HST images provides a rough approximation for the relative SFR distribution. In the MUSE-Deep UDF fields we use the deep HST F775W imaging. In all other fields we use the F814W band. Although ideally we would like to use photometry that covers the rest-frame ultraviolet light in each galaxy, the necessary deep multiwavelength HST imaging does not exist for all fields. To strike a good balance, we use the F775W and F814W filters, since they are providing the S/N required. This has the additional advantage that, because these filters have similar pivot wavelengths, we also ensure a degree of consistency between the fields. We construct SFR maps of our galaxies by cropping the HST images to only include flux within an ellipse of radius 4 × r d along the major axis. This ellipse has the same morphology (RA, Dec, inc., PA) as above. We inspect each image and alter the mask if necessary to ensure that we include all flux from the object and to remove other objects or defects. When necessary, we interpolate over these rather than mask them. Negative flux values are set to zero. The final result is an SFR map that represents the relative spatial distribution of the SFR. The absolute SFR values are determined by normalizing the map to the total SFR, SFR tot , which is a free parameter in the model. From experience with our C17 work, we found that it was quite important to include the complex spatial variations of the SFR in our model. Using an SFR map (as opposed to simply assuming an exponential disc) appeared to improve the accuracy of our model. However, including an SFR map does not correct for all effects of clumpy star formation. Indeed, a limitation of our model is that, by construction, we do not accommodate for galaxies with strong azimuthal metallicity variations 12 ; we should anticipate that we may observe galaxies where the bright star-forming clumps have uncharacteristically low/high metallicities. However, it should be noted that, for the low-redshift galaxies where azimuthal metallicity variations have been quantified, the variations are typically found to be quite small (≲0.05 dex; e.g. Sánchez et al. 2015 ; Zinchenko et al. 2016 ; Sánchez-Menguiano et al. 2017 ), and there is only the odd example of a galaxy with variations as large as ≈0.2 dex (e.g. Vogt et al. 2017 ). That said, even if there were large azimuthal variations in our galaxies, it does not mean that we cannot still make inferences in these cases because, in effect, we likely still measure the radial metallicity profile of brightest star-forming regions (i.e. a quasi flux-weighted metallicity profile). Nevertheless, this would be in contrast with