cosmic evolution is through the spherically-averaged distance, $D_V$, with mixed information from both modes [@Eisenstein05].

Alternatively, we follow a [*quasi*]{} model-independent approach to measure the transversal BAO mode at high redshift, and for this we consider a sample of quasars located in a thin range of redshift of the SDSS DR12 dataset [@Paris]. The main idea behind this approach is that, if the redshift bin is sufficiently thin then the two-point angular correlation function (2PACF), calculated over the angular coordinates without using a fiducial cosmological model, successfully captures the transversal BAO mode. Rigorously, this procedure is [*quasi*]{} model-independent because a cosmological model is used just in two steps [@Sanchez11; @Carnero; @Carvalho; @Salazar; @Alcaniz]: (i) the transversal BAO analysis is done in a thin but finite redshift bin, i.e., $\delta z \ne 0$, and therefore there is a small shift in the BAO angular position; however, for the quasar sample studied here, in which $\delta z = 0.05$, the shift correction is only $0.9\%$ of the BAO measured scale (as we shall show); (ii) the comoving sound horizon, $r_{s}$, used to calculate the angular diameter distance from the BAO angular position, $D_A$, is obtained assuming a cosmological model (see, e.g., [@Heavens; 