  We studied the WMAP temperature anisotropy data using two different methods.
The derived signal gradient maps show regions with low mean gradients in
structures near the ecliptic poles and higher gradient values in the wide
ecliptic equatorial zone, being the result of non-uniform observational time
sky coverage. We show that the distinct observational time pattern present in
the raw (cleaned) data leaves also its imprints on the composite CMB maps.
Next, studying distribution of the signal dispersion we show that the
north-south asymmetry of the WMAP signal diminishes with galactic altitude,
confirming the earlier conclusions that it possibly reveals galactic foreground
effects. As based on these results, one can suspect that the instrumental noise
sky distribution and non-removed foregrounds can have affected some of the
analyses of the CMB signal. We show that actually the different characteristic
axes of the CMB sky distribution derived by numerous authors are preferentially
oriented towards some distinguished regions on the sky, defined by the
observational time pattern and the galactic plane orientation.
