  A new and promising technique for observing the Universe and study the dark
sector is the intensity mapping of the redshifted 21cm line of neutral hydrogen
(HI). The BINGO radio telescope will use the 21cm line to map the Universe in
the redshift range $0.127 \le z \le 0.449$, in a tomographic approach, with the
main goal of probing BAO. This work presents the forecasts of measuring the
transversal BAO signal during the BINGO Phase 1 operation. We use two
clustering estimators, the two-point angular correlation function (ACF) and the
angular power spectrum (APS), and a template-based method to model the ACF and
APS estimated from simulations of the BINGO region and extract the BAO
information. The tomographic approach allows the combination of redshift bins
to improve the template fitting performance. We find that each clustering
estimator shows different sensitivities to specific redshift ranges, although
both of them perform better at higher redshifts. In general, the APS estimator
provides slightly better estimates, with smaller uncertainties and larger
probability of detection of the BAO signal, achieving $\gtrsim 90$\% at higher
redshifts. We investigate the contribution from instrumental noise and residual
foreground signals and find that the former has the greater impact, getting
more significant as the redshift increases, in particular the APS estimator.
Indeed, including noise in the analysis increases the uncertainty up to a
factor of $\sim 2.2$ at higher redshifts. Foreground residuals, in contrast, do
not significantly affect our final uncertainties. In summary, our results show
that, even including semi-realistic systematic effects, BINGO has the potential
to successfully measure the BAO scale in radio frequencies. (Abridged)
