Determining cosmic microwave background anisotropies in the presence of foregrounds

Details Determining cosmic microwave background anisotropies in the presence of foregrounds Determining cosmic microwave background anisotropies in the presence of foregrounds

1995-12-05

arxiv.org/abs/astro-ph/9512021v1

Astrophys.J. 482 (1997) 577

Astronomy and Astrophysics

Astrophysics

25 pages LaTex and 8 postscript figures, uses psfig.tex. Color postscript version with embedded figures available at http://

Scientific paper

10.1086/304157

Separating foregrounds from the signal is one of the big challenges in cosmic microwave background (CMB) experiments. A simple way to estimate the CMB temperature in a given pixel is to fit for the amplitudes of the CMB and the various foreground components. The variance squared of this estimator is shown to be equal to $[(FDF)^2\ \sigzt + \sigsh^2]$, where $\sigz$ is the variance in the absence of foregrounds; $\sigsh$ is the variance due to the uncertainty in the shapes of the foreground components; and FDF is the {\it foreground degradation factor}. This one number, the FDF, gives a good indication of the ability of a given experiment to disentangle the CMB from foreground sources. A variety of applications relating to the planning and analyzing of experiments is presented.

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