Notes. For the MUSE lines, we give the FWHM, which has been corrected in quadrature using the instrument resolution of ∼110 km s⁻¹ at ∼1550 Å. In the southern region, the [C I] flux is a 3σ upper limit. ^( ⋆ )The minimum Lyα flux is estimated by integrating over the wavelength range where the emission should be, excluding the wavelength ranges affected by sky lines (yellow regions in Fig. 4). At the core of 4C 19.71, the blue side is completely absorbed and dominated by sky-subtraction residuals from the strong 5577Å sky line; the integrated flux is thus a lower limit since we are missing a significant portion of the likely emission. ^( † )Fit to the Lyα line excluding the wavelengths impacted by the night sky residuals. These fits are shown as the dashed red line in Fig. 4. We note that these estimates are likely to only be accurate to the order-of-magnitude level given the limited range of the profile that is not impacted by the strong night sky line at these wavelengths. ^{( ⋆ ⋆)}The He II line is severely affected by sky line noise and residuals and cannot be fitted with any certainty. Instead, the integrated flux is estimated by scaling a Gaussian with the same width and velocity offset as the C IV line, and for flux ratios He II/C IV = 0.5, 1, and 2 for the northern component and He II/C IV = 2 and 3 for the southern component, as indicated in Fig. 4.