Posterior probability distribution obtained from BEAGLE, illustrating the subset of model parameters most relevant to this work. From left to right, the effective V-band dust attenuation optical depth ${\widehat{\tau }}_{\mathrm{V}}$, ionisation parameter log (U), dust-to-metal mass ratio ξ_d, gas-phase metallicity 12 + log (O/H), C/O abundance (in logarithmic units of the solar C/O abundance), and predicted line ratio C III]/([O II]+[Ne III]), which is the main empirical constraint coming from the NIRSpec spectrum. The analysis with BEAGLE suggests that our data are best reproduced by models with slightly super solar C/O abundance. The inset diagram shows the NIRSpec data (red) and their uncertainties (light red), as well as the model predictions from BEAGLE (in blue the posterior median, while the shaded light blue region indicates the 68% credible region). The bottom panel shows the residual in units of σ, the observational error, with the grey band encompassing ±1 σ. We mask the region around Lyα, since we do not model this line self-consistently.