WMAP data when combined with ancillary data on free-free , synchrotron and dust allow an improved understanding of the spectrum of emission from each of these components .
Here we examine the sky variation at intermediate and high latitudes using a cross-correlation technique .
In particular , we compare the observed emission in several large partitions of the sky plus 33 selected sky regions to three “ standard ” templates .
The regions are selected using a criterion based on the morphology of these template maps .

The synchrotron emission shows evidence of steepening between GHz frequencies and the WMAP bands .
There are indications of spectral index variations across the sky but the current data are not precise enough to accurately quantify this from region-to-region .

The emission correlated with the H _ { \alpha } template shows clear evidence of deviation from a free-free spectrum .
The emission can be decomposed into a contribution from both free-free and spinning dust in the warm ionised medium of the Galaxy .
The derived free-free emissivity corresponds to a mean electron temperature of \sim 6000 K , although the value depends critically on the impact of dust absorption on the H _ { \alpha } intensity .
The WIM spinning dust emission has a peak emission in intensity in the range 40–50 GHz .

The anomalous microwave emission associated with dust is detected at high significance in most of the 33 fields studied .
The anomalous emission correlates well with the Finkbeiner et al .
( 1999 ) model 8 predictions ( FDS8 ) at 94 GHz , and is well described globally by a power-law emission model with an effective spectral index between 20 and 60 GHz of \beta \approx - 2.7 .
It is clear that attempts to explain the emission by spinning dust models require multiple components , which presumably relates to a complex mix of emission regions along a given line-of-sight .
An enhancement of the thermal dust contribution over the FDS8 predictions by a factor \sim 1.2 is required with such models .
Furthermore , the emissivity varies by a factor of \sim 50 \% from cloud to cloud relative to the mean .

The significance of these results for the correction of CMB data for Galactic foreground emission is discussed .