Notes. These results confirm 29/45 sources (64.4%) as genuine Lyα ​-emitting QSOs at z​ ∼ ​2. The most numerous interlopers are CIV-emitting QSOs at z​ ∼ ​1.52, namely 8/45 targets (∼18%, see Stroe et al. 2017a,b), and 5/45 blue stars (∼11%). The latter are selected by our pipeline due to their strong colour-gradients which mimic a NB photometric excess in the J0395 filter. We also note one Lyβ-emitting QSO contaminant at z​ ∼ ​2.76. We report the measured L_Lyα and EW_obs only for the confirmed QSOs at z​ ∼ ​2.2. Among these, the spectrum of GTC 16 could not be calibrated and measured. Finally, all the z​ ∼ ​2.2 confirmed sources in our sample are QSOs with L_Lyα​ >  ​6 × 10⁴³ erg s⁻¹. This supports the results of Konno et al. (2016), Matthee et al. (2017b), Sobral et al. (2018b,a) and Calhau et al. (2020) about the strong contribution of AGNs/QSOs to the Lyα LF at Log(Lyα)​ ≳ ​43.3.