Separating foregrounds from the signal is one of the major challenges
in cosmic microwave background (CMB) experiments. A simple way to esti
mate the CMB temperature in a given pixel is to fit for the amplitudes
of the CMB and the various foreground components. The variance square
d of this estimator is shown to be equal to (FDF)(2) sigma(theta)((0)2
) + sigma(shape)(2)s where sigma(theta)((0)) is the variance in the ab
sence of foregrounds, sigma(shape) is the variance due to the uncertai
nty in the shapes of the foreground components, and FDF is the foregro
und degradation factor. This one number, the FDF, gives a good indicat
ion of the ability of a given experiment to disentangle the CMB from f
oreground sources. A variety of applications relating to the planning
and analyzing of experiments is presented. This approach, viz., analyz
ing the variance, can be used to assess the usefulness of any estimato
r.