map the monopole and dipole components, and the spectral components cased by the Galaxy emission. Then the sum map is additionally “cleaned” from the Galactic radiation. For this purpose we use 19 GHz and 31 GHz maps to determine the Galactic radiation spectral index. Then the 31 GHz map is subtracted from 53 GHz map, but with a weight corresponding the determined spectral index.

We assume the hypothesis the cosmological signal and the noise are normal distributed. The noise spectrum shape is assumed to be completely determined by the number of measurements in every point on the sky. Based on this we calculate the noise parameters and discover anomalous noise components. Then we use a Monte Carlo simulation to estimate signal magnitude, signal spectrum parameters, and the estimates confidence levels. The latter procedure is applied both to a total analyzed spectrum and to a censored spectrum with anomalous components excluded. In addition we test the determined estimations for stability to the procedure of quadrupole component subtracting.

 Signal Analysis on the Sphere.
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The signal on the sphere may be represented as a spherical harmonics expansion $Y_{l,m}(\theta, \varphi)$: $$\Delta T(\theta, \varphi)  = \sum a^m_l Y_{l,m}(\theta, \varphi)$$ In this case the signal 