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We present an analysis of the foreground emission present in the WMAP 3-yeardata as determined by the method of Independent Component Analysis. We derivedcoupling coefficients between the WMAP data and foreground templates which arethen used to infer the spectral behaviour for three foreground components --synchrotron, anomalous dust-correlated emission and free-free. For the firsttwo components, we find values consistent with previous results althoughslightly steeper. We confirm the inconsistency in the scaling between the Hatemplate and free-free emission at K- and Ka-bands where an electrontemperature of ~ 4000 K is indicated. We also see evidence of significantlyflatter spectral behaviour to higher frequencies than expected theoreticallyand previously noted by Dobler et al.(2008a), but only when analysing the Kp2sky coverage. We further apply FASTICA 'iteratively', using data pre-cleanedusing foreground templates scaled to the WMAP frequencies by couplingcoefficients determined by a prior FASTICA analysis. This multi-frequencyanalysis allows us to determine the presence of residual foreground emissionnot traced by the templates. We confirm the existence of a component spatiallydistributed along the Galactic plane and particularly enhanced near the center(the 'WMAP haze'). This emission is less extended when using the WMAP K-Ka dataas the synchrotron template confirming that it can be considered a bettertemplate for foreground cleaning of the WMAP data. However its use complicatesthe physical interpretation of the nature of the foreground emission andresiduals. since it contains a mixture of several, physically distinct emissionmechanisms.

Foreground analysis of the WMAP three-year data with FASTICA