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The purpose of this work is to characterize the diffuse Galactic polarizedsynchrotron, which is the dominant CMB foreground emission at low frequency. Wepresent EE, BB, and EB power spectra estimated from polarization frequency mapsat 23 and 30 GHz as observed respectively by the WMAP K-band and the Plancklowest frequency channel, for a set of six sky regions covering from 30% to 94%of the sky. We study the synchrotron polarization angular distribution andspectral energy distribution (SED) by means of the so-called pseudo-$C_\ell$formalism, provided by the NaMaster package, in the multipole interval 30$\leq$ $\ell$ $\leq$ 300. Best results are obtained cross-correlating Planckand WMAP data. The EE and BB angular power spectra show a steep decay of thespectral amplitude as a function of multipole, approximated by a power law$C^{EE,BB} \propto \ell^{\alpha_{EE,BB}}$, with $\alpha_{EE}= -2.95\pm0.04$ and$\alpha_{BB}=-2.85\pm0.14$. The B/E power asymmetry is proved with a B-to-Eratio, computed as the amplitude ratio at the pivot multipole $\ell = 80$, of0.22$\pm$0.02. The EB cross-component is compatible with zero at 1$\sigma$,with an upper constraint on the EB/EE ratio of 1.2% at the 2$\sigma$ level. Weshow that the EE and BB power-law model with null EB cross-correlationdescribes reasonably well the diffuse synchrotron polarization emission for thefull sky if the bright Galactic center and point sources are masked. Therecovered SED shows power-law spectral indices $\beta_{EE}= -3.00 \pm 0.10$ and$\beta_{BB} = -3.05\pm0.36$ compatible between themselves, in the frequencyrange 23-30 GHz. Results also seem to indicate that the SED gets steeper fromlow to high Galactic latitude.

Characterization of the polarized synchrotron emission from Planck and WMAP data