This paper investigates the redshift dependence of the Hubble tension by comparing luminosity distances derived from BAO data (calibrated with the CMB-inferred sound horizon) and Pantheon+ SnIa data (calibrated with Cepheids). The analysis uses redshift tomography to examine discrepancies between these distance measurements across different redshift bins. The results show that BAO-inferred distances are inconsistent with Pantheon+ SnIa distances across all redshift bins, with the discrepancy being more pronounced at lower redshifts (z ∈ [0.1, 0.8]) than at higher redshifts (z ∈ [0.8, 2.3]). The consistency of ΛCDM best-fit parameters in low and high redshift bins is investigated, and the tension is found to reduce at higher redshifts. However, a mild tension is identified between redshift bins at higher redshifts for both BAO and Pantheon+ data, consistent with previous studies suggesting an evolution of H₀ in the ΛCDM framework. The findings indicate that low-redshift BAO and SnIa distances can only become consistent through a re-evaluation of distance calibration methods. An H(z) expansion rate deformation alone is insufficient to resolve the tension. The study also hints at a possible deviation of the expansion rate from the Planck18/ΛCDM model at high redshifts (z ≥ 2). The results suggest that a high-redshift transition in H(z), as in the Λ_s CDM model, may provide a better fit to SnIa data, although it does not fully resolve the Hubble tension due to inconsistencies with intermediate/low z BAO data. The analysis highlights the need for further investigation into the redshift dependence of the Hubble tension and the potential role of systematic effects in the data.This paper investigates the redshift dependence of the Hubble tension by comparing luminosity distances derived from BAO data (calibrated with the CMB-inferred sound horizon) and Pantheon+ SnIa data (calibrated with Cepheids). The analysis uses redshift tomography to examine discrepancies between these distance measurements across different redshift bins. The results show that BAO-inferred distances are inconsistent with Pantheon+ SnIa distances across all redshift bins, with the discrepancy being more pronounced at lower redshifts (z ∈ [0.1, 0.8]) than at higher redshifts (z ∈ [0.8, 2.3]). The consistency of ΛCDM best-fit parameters in low and high redshift bins is investigated, and the tension is found to reduce at higher redshifts. However, a mild tension is identified between redshift bins at higher redshifts for both BAO and Pantheon+ data, consistent with previous studies suggesting an evolution of H₀ in the ΛCDM framework. The findings indicate that low-redshift BAO and SnIa distances can only become consistent through a re-evaluation of distance calibration methods. An H(z) expansion rate deformation alone is insufficient to resolve the tension. The study also hints at a possible deviation of the expansion rate from the Planck18/ΛCDM model at high redshifts (z ≥ 2). The results suggest that a high-redshift transition in H(z), as in the Λ_s CDM model, may provide a better fit to SnIa data, although it does not fully resolve the Hubble tension due to inconsistencies with intermediate/low z BAO data. The analysis highlights the need for further investigation into the redshift dependence of the Hubble tension and the potential role of systematic effects in the data.