Hubble tension tomography: BAO vs SN Ia distance tension

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+SN Ia distances calibrated with Cepheids. Using a redshift tomography method. We find: (1) The BAO-inferred distances are discrepant with the Pantheon+SN Ia distances across all redshift bins considered, with the discrepancy level varying with redshift. (2) The distance discrepancy is more pronounced at lower redshifts (z0. 1, 0. 8) compared to higher redshifts (z0. 8, 2. 3). The consistency of best fit parameters obtained in high and low redshift bins of both BAO and SN Ia 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 H₀ in agreement with previous studies which find hints for an ``evolution'' of H₀ in the context of. These results confirm that the low redshift BAO and SN Ia distances can only become consistent through a reevaluation 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/ model at high redshifts z2. We show that such a deformation is well described by a high redshift transition of H (z) like the one expressed by ₒCDM even though this alone cannot fully resolve the Hubble tension due to its tension with intermediate/low z BAO data.