The so-called “cosmic dipole tension” challenges the cosmological principle by positing a discrepancy between the Solar System’s peculiar velocity inferred from the cosmic microwave background (CMB) dipole and that derived from large-scale structure number-count dipoles. Here we provide a high-precision determination of the kinematic dipole using the redshift-dipole method applied to the first data release (DR1) of the dark energy spectroscopic instrument (DESI). By exploiting the Doppler-induced modulation of observed redshifts, this estimator is intrinsically less sensitive to imaging systematics and selection-function uncertainties that can bias traditional number-count measurements. We conduct a tomographic analysis of four tracer populations, bright galaxy sample, luminous red galaxies, emission line galaxies, and quasars, spanning $0.1<z<2.1$. Survey geometry and statistical uncertainties are quantified using 1000 EZmock realizations. We find that the high-redshift QSO sample implies a peculiar velocity of $v={357.95}_{-48.47}^{+55.05}\mathrm{km}{\mathrm{s}}^{-1}$, in excellent agreement with the CMB-inferred value of $369.82\pm 0.11\mathrm{km}{\mathrm{s}}^{-1}$. By contrast, a complementary number-count analysis yields a significantly enhanced dipole amplitude, which we attribute to leakage of large-scale power and to incompleteness within the DESI DR1 footprint. These results indicate that the redshift dipole provides a cleaner and more reliable probe of the kinematic rest frame, offering strong support for the standard kinematic interpretation at high redshift and helping to resolve the apparent dipole anomaly.

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• Large scale structure of the Universe