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We present Cosmoglobe Data Release 1, which implements the first jointanalysis of WMAP and Planck LFI time-ordered data, processed within a singleBayesian end-to-end framework. This framework builds directly on a similaranalysis of the LFI measurements by the BeyondPlanck collaboration, andapproaches the CMB analysis challenge through Gibbs sampling of a globalposterior distribution, simultaneously accounting for calibration, mapmaking,and component separation. The computational cost of producing one completeWMAP+LFI Gibbs sample is 812 CPU-hr, of which 603 CPU-hrs are spent on WMAPlow-level processing; this demonstrates that end-to-end Bayesian analysis ofthe WMAP data is computationally feasible. We find that our WMAP posterior meantemperature sky maps and CMB temperature power spectrum are largely consistentwith the official WMAP9 results. Perhaps the most notable difference is thatour CMB dipole amplitude is $3366.2 \pm 1.4\ \mathrm{\mu K}$, which is $11\\mathrm{\mu K}$ higher than the WMAP9 estimate and $2.5\ {\sigma}$ higher thanBeyondPlanck; however, it is in perfect agreement with the HFI-dominated PlanckPR4 result. In contrast, our WMAP polarization maps differ more notably fromthe WMAP9 results, and in general exhibit significantly lower large-scaleresiduals. We attribute this to a better constrained gain and transmissionimbalance model. It is particularly noteworthy that the W-band polarization skymap, which was excluded from the official WMAP cosmological analysis, for thefirst time appears visually consistent with the V-band sky map. Similarly, thelong standing discrepancy between the WMAP K-band and LFI 30 GHz maps isfinally resolved, and the difference between the two maps appears consistentwith instrumental noise at high Galactic latitudes. All maps and the associatedcode are made publicly available through the Cosmoglobe web page.

Cosmoglobe DR1 results. I. Improved Wilkinson Microwave Anisotropy Probe maps through Bayesian end-to-end analysis