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We present the first model of full-sky polarized synchrotron emission that is derived from all WMAP and Planck LFI frequency maps. The basis of this analysis is the set of end-to-end reprocessed C OSMOGLOBE Data Release 1 (DR1) sky maps presented in a companion paper, which have significantly lower instrumental systematics than the legacy products from each experiment. We find that the resulting polarized synchrotron amplitude map has an average noise rms per 2° full width at half maximum (FWHM) beam of 3.2 μK at 30 GHz. This is 30% lower than the recently released B EYOND P LANCK model that included only LFI+WMAP Ka – V data, and 29% lower than the WMAP K -band map alone. The mean B -to- E power spectrum ratio is 0.39 ± 0.02, with amplitudes consistent with those measured previously by Planck and QUIJOTE. Assuming a power law model for the synchrotron spectral energy distribution and using the T – T plot method, we find a full-sky inverse noise-variance-weighted mean of the synchrotron polarized spectral index of β s = −3.07 ± 0.07 from the C OSMOGLOBE DR1 K band and 30 GHz, in good agreement with previous estimates. In summary, the novel C OSMOGLOBE DR1 synchrotron model is both more sensitive and systematically cleaner than similar previous models, and it has a more complete error description that is defined by a set of Monte Carlo posterior samples. We believe that these products are preferable over previous Planck and WMAP products for all synchrotron-related scientific applications, including simulations, forecasting, and component separation.
Watts et al. (Fri,) studied this question.