  The main goals of this study is to use the information from both WMAP
intensity and polarization data to do a separation of the Galactic components,
with a focus on the synchrotron and anomalous emissions. Our analysis is made
at 23 GHz where the signal-to-noise ratio is the highest and the estimate of
the CMB map is less critical. Our estimate of the synchrotron intensity is
based on an extrapolation of the Haslam 408 MHz data with a spatially varying
spectral index constrained by the WMAP 23 GHz polarization data and a
bi-symmetrical spiral model of the galactic magnetic field with a turbulent
part following a -5/3 power law spectrum. The 23 GHz polarization data are
found to be compatible with a magnetic field with a pitch angle p=-8.5 degrees
and an amplitude of the turbulent part of the magnetic field 0.57 times the
local value of the field, in agreement with what is found using rotation
measures of pulsars and polarized extinction by dust. The synchrotron spectral
index between 408 MHz and 23 GHz obtained from polarization data and our model
of the magnetic field has a mean value of Beta=-3.00 with a limited spatial
variation with a standard deviation of 0.06. When thermal dust, free-free and
synchrotron are removed from the WMAP intensity data, the residual anomalous
emission is highly correlated with thermal dust emission with a spectrum in
agreement with spinning dust models. Considering a classical model of the large
scale Galactic magnetic field, we show that the polarization data of WMAP are
in favor of a soft synchrotron intensity highly correlated with the 408 MHz
data. Furthermore the combination of the WMAP polarization and intensity data
brings strong evidence for the presence of unpolarized spinning dust emission
in the 20-60 GHz range.
