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We present a new approach to foreground removal for Cosmic MicrowaveBackground (CMB) maps. Rather than relying on prior knowledge about theforeground components, we first extract the necessary information about themdirectly from the microwave sky maps by taking differences of temperature mapsat different frequencies. These difference maps, which we refer to as internaltemplates, consist only of linear combinations of galactic foregrounds andnoise, with no CMB component. We obtain the foreground cleaned maps by fittingthese internal templates to, and subsequently subtracting the appropriatelyscaled contributions of them from, the CMB dominated channels. The fittingoperation is performed in wavelet space, making the analysis feasible at highresolution with only a minor loss of precision. Applying this procedure to theWMAP data, we obtain a power spectrum that matches the spectrum obtained by theWMAP team at the signal dominated scales. Finally, we have revisited previousclaims about a north-south power asymmetry on large angular scales, and confirmthat these remain unchanged with this completely different approach toforeground separation. This also holds when fitting the foreground contributionindependently to the northern and southern hemisphere indicating that theasymmetry is unlikely to have its origin in different foreground properties ofthe hemispheres. This conclusion is further strengthened by the lack of anyobserved frequency dependence.Comment: Submitted to Ap

Foreground Subtraction of Cosmic Microwave Background Maps Using WI‐FIT (Wavelet‐Based High‐Resolution Fitting of Internal Templates)