The paper investigates the redshift dependence of the Hubble tension by comparing luminosity distances derived from an up-to-date BAO dataset (including the latest DESI data) calibrated with the CMB-inferred sound horizon, and Pantheon+ SnIa distances calibrated with Cepheids. Using a redshift tomography method, the authors find that: 1. The BAO-inferred distances are discrepant with the Pantheon+ SnIa distances across all redshift bins, with the discrepancy varying with redshift. 2. The distance discrepancy is more pronounced at lower redshifts ($z \in [0.1, 0.8]$) compared to higher redshifts ($z \in [0.8, 2.3]$). 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 it is confirmed that the tension reduces at high redshifts. 4. A mild tension between redshift bins is identified at higher redshifts for both BAO and Pantheon+ data with respect to the best-fit value of $H_0$, consistent with previous studies suggesting 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. The findings also hint at a possible deviation of the expansion rate from the Planck18/ACDM model at high redshifts ($z \gtrsim 2$), which is well described by a high-redshift transition of $H(z)$ like the one expressed by $\Lambda_c$CDM. However, this deformation alone cannot fully resolve the Hubble tension due to its tension with intermediate/low $z$ BAO data.The paper investigates the redshift dependence of the Hubble tension by comparing luminosity distances derived from an up-to-date BAO dataset (including the latest DESI data) calibrated with the CMB-inferred sound horizon, and Pantheon+ SnIa distances calibrated with Cepheids. Using a redshift tomography method, the authors find that: 1. The BAO-inferred distances are discrepant with the Pantheon+ SnIa distances across all redshift bins, with the discrepancy varying with redshift. 2. The distance discrepancy is more pronounced at lower redshifts ($z \in [0.1, 0.8]$) compared to higher redshifts ($z \in [0.8, 2.3]$). 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 it is confirmed that the tension reduces at high redshifts. 4. A mild tension between redshift bins is identified at higher redshifts for both BAO and Pantheon+ data with respect to the best-fit value of $H_0$, consistent with previous studies suggesting 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. The findings also hint at a possible deviation of the expansion rate from the Planck18/ACDM model at high redshifts ($z \gtrsim 2$), which is well described by a high-redshift transition of $H(z)$ like the one expressed by $\Lambda_c$CDM. However, this deformation alone cannot fully resolve the Hubble tension due to its tension with intermediate/low $z$ BAO data.