Derived Lyα+N V emission line properties of the discovered quasars. Left: normalised Lyα+N V EW distribution of the discovered quasars in this work compared to the distribution of PS1 discovered quasars at z >  5.6 by Bañados et al. (2016) and SDSS discovered quasars at z >  3 by Diamond-Stanic et al. (2009). Our EW distribution is consistent with the optically selected quasars sample of Bañados et al. (2016). Right: Lyα+N V luminosity versus the radio luminosity at 144 MHz for the quasars in this work, showing little to no correlation (see Sect. 5.3).