Quasar-subtracted spectra integrated over the three spatial regions shown in Figure 3 (opaque coloured lines) along with our best-fit Gaussian models for the Hβ and [O III] λλ4959,5007 emission lines (black). The analogous spectra from the non-quasar-subtracted cube are also plotted for comparison (transparent coloured lines), showing the necessity of quasar subtraction to accurately measure the emission from Regions 1 and 2. All spectra have been continuum subtracted. The vertical lines mark the location of the Hβ and [O III] λλ4959,5007 lines at the redshift of the quasar host galaxy, Region 1, as measured from the fit to this spectrum, z = 7.0804 ± 0.0028. For the host Region 1, we exclude the central 5 × 5 pixels surrounding the quasar peak as well as nearby spaxels with [O III] λ5007 velocity offset > 300 km/s, as these are highly corrupted by the quasar subtraction and introduce significant noise and artefacts. This means that we slightly underestimate the total flux in this region; however, the fluxes are significantly more reliable than if these most corrupted spaxels were included.