54.82 \, \mu{\rm K}$.

The same analysis, but without excluding anomalous components shows two estimates:

$\sigma_{Tenerif} = 37.22 \, \mu{\rm K}$ with quadrupole included, and: $\sigma_{Tenerif} = 34.47 \, \mu{\rm K}$ with quadrupole excluded.

We do not use a $4^{\circ}$ binning in the analysis. The binning may decrease the obtained data in some degree. The binning is used in Tenerife experiment and the results are (Hancock S. et al., 1994):

$\sigma_s=49\pm 10 \, \mu{\rm K}$ for 33 GHz channel, and $\sigma_s=42\pm 9 \, \mu{\rm K}$ for a sum of the 15 and 31 GHz channels. So the cosmological signal spectrum with the parameters we obtained is in a good agreement with the observations which are more sensitive than COBE for high spatial harmonics.

 Conclusions.
=============

The systematic effects exclusion problem is met practically in any experiment. In the case of CMB anisotropy observation the Galaxy radiation is the primary effect. The method usually used to suppress the radiation is to “cut off” the Galaxy plane region. It causes the problem of the monopole and dipole exclusion. The latter in its turn effects the additional systematic errors but at the less level.

The orthogonal basis when coupled with the spatial-frequency filtering 