  We investigate the redshift dependence of the Hubble tension by comparing the
luminosity distances obtained using an up-to-date BAO dataset (including the
latest DESI data) calibrated with the CMB-inferred sound horizon, and the
Pantheon+ SnIa distances calibrated with Cepheids. Using a redshift tomography
method, we find: 1) The BAO-inferred distances are discrepant with the
Pantheon+ SnIa distances across all redshift bins considered, with the
discrepancy level varying with redshift. 2) The distance discrepancy is more
pronounced at lower redshifts ($z \in [0.1,0.8]$) compared to higher redshifts
($z\in [0.8,2.3]$). The consistency of $\Lambda$CDM best fit parameters
obtained in high and low redshift bins of both BAO and SnIa samples is
investigated and we confirm that the tension reduces at high redshifts. Also a
mild tension between the redshift bins is identified at higher redshifts for
both the BAO and Pantheon+ data with respect to the best fit value of $H_0$ in
agreement with previous studies which find hints for an 'evolution' of $H_0$ in
the context of $\Lambda$CDM. These results confirm that the low redshift BAO
and SnIa distances can only become consistent through a re-evaluation of the
distance calibration methods. An $H(z)$ expansion rate deformation alone is
insufficient to resolve the tension. Our findings also hint at a possible
deviation of the expansion rate from the Planck18/$\Lambda$CDM model at high
redshifts $z\gtrsim 2$. We show that such a deformation is well described by a
high redshift transition of $H(z)$ like the one expressed by $\Lambda_s$CDM
even though this alone cannot fully resolve the Hubble tension due to its
tension with intermediate/low $z$ BAO data.
