  Understanding the statistical properties of synchrotron emission from our
Galaxy is valuable from the perspective of observations targeting signals of
cosmological origin, as well as for understanding physical processes in our
Galaxy. In this work, we extend the analysis of arXiv:2104.00419v2 to -- (a)
all-sky observed maps of total foreground emissions at different frequencies
provided by WMAP, Planck and Stockert-Villa, (b) component separated
synchrotron temperature maps provided by WMAP, Planck and BeyondPlanck, and (c)
component separated polarization maps provided by WMAP and Planck. The tools we
use are Minkowski functionals and tensors. Our main goals are twofold. First,
we determine the variation of morphological properties of the total foreground
maps with observing frequency and compare with simulations. This elucidates how
the morphology varies due to the relative dominance of different foreground
components at different frequencies. Next, we analyze the nature of
non-Gaussianity and statistical isotropy of synchrotron fluctuations on smaller
scales using various component separated synchrotron temperature and
polarization maps. We find that all maps exhibit kurtosis non-Gaussianity, in
agreement with the Haslam map. This result can be an important input for the
modelling of small-scale synchrotron fluctuations for component separation
pipelines. This also suggests that residual synchrotron contamination in CMB
will manifest as kurtosis. Studying different component separated maps, we find
that BeyondPlanck and WMAP MCMC-e agree well with Haslam at all scales. The
other maps show differences of varying statistical significance. Our analysis
suggests a combination of residual AME and/or free-free emissions and point
sources as contributing to these differences, and underscores the need for
further improvement of the pipelines.
