\[bin-size\] and \[errors\] that the BAO signal is also robust under different bin-size choices, $N_{b}$, used in the calculation of the 2PACF and the corresponding BAO scale measurement. Additionally, we verify in section \[sec:small\_shift\] that our measurement is stable under small Gaussian random perturbations of the angular positions of the quasars sample (this is a useful procedure which also leads to discriminate possible noise bumps from the true BAO signature).

With this angular BAO measurement we have increased the number of available BAO angular scale data, this time with a measurement at high redshift. We combined this new measurement with other eight data points (from refs. [@Carvalho; @Alcaniz]) to constrain the cosmological parameters of wCDM and w$(a)$CDM models. Our results show an excellent agreement with the standard cosmological model $\Lambda$CDM: the best-fit corresponds to $\Omega_m= 0.31 \pm 0.02$ and w$_0 = -0.92 \pm 0.06$ for the wCDM model, while for w$(a)$CDM we found w$_0= -0.87 \pm 0.13$ and w$_a= -0.15 \pm 0.32$ (see figure \[contours\] and section \[CC\] for details).

Moreover, it is worth emphasizing that our likelihood analyses considers the covariance matrices sourced by linear and non-linear analytical power spectra, finding a negligible difference between both cases, an expected 