plane and the Galaxy center are excluded from the total spatial spectrum. By this expedient the Galactic radiation magnitude is essentially reduced. And only after that, during the second filtering stage a “frequency cleaning” procedure is used. At this stage the CMB anisotropy is separated from the Galactic radiation using several frequency channels and some a priori Galaxy radiation model. The both stages nowhere are associated with any signal harmonics orthogonality losses.

The main method difficulty may be found at the second stage and is bound up with the problem of a correct Galactic radiation model selection. But using the first stage filtering we strongly reduce the effect of the model uncertainty on the net result.

As an initial data we used public released COBE DMR 2-years all sky maps from 31.5, 53, and 90 GHz frequency channels. In addition we exploited a 19.2 GHz balloon data kindly provided by the authors of the survey.

 The Method.
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A data reduction process practically always is accomplished by some types of the data censoring like weighing, excluding outliers, corrections for systematic errors, trends and so on. A censor method selection is based on a priori information about the analyzing sample. The 