Comparison of the BLR profiles of the C IV (from Shen 2016) and Hα and Hβ (from the integrated NIRSpec spectrum), in velocity space. For the Balmer lines, we also report the best-fit BLR profiles. All line profiles have been normalised to the flux of the BLR component in the reddest parts, which are likely less affected by BLR and NLR outflows. The C IV shows a significant excess in the blue part, at velocities of a few thousand km s⁻¹, which is not observed in the Balmer lines or in the [O III] line. This excess possibly indicates strong BLR winds.