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B-modes of Cosmic Microwave Background (CMB) polarization can be created by aprimordial gravitational wave background. If this background was created byInflation, then the amplitude of the polarization signal is proportional theenergy density of the universe during inflation. The primordial signal will becontaminated by polarized foregrounds including dust and synchrotron emissionwithin the galaxy. In light of the WMAP polarization maps, we consider theability of several hypothetical CMB polarization experiments to separateprimordial CMB B-mode signal from galactic foregrounds. We also study theoptimization of a CMB experiment with a fixed number of detectors in the focalplane to determine how the detectors should be distributed in differentfrequency bands to minimize foreground confusion. We show that the optimalconfiguration requires observations in at least 5 channels spread over thefrequency range between 30 GHz and 500 GHz with substantial coverage around 150GHz. If a low-resolution space experiment using 1000 detectors to reach a noiselevel of about 1000 nK$^2$ concentrates on roughly 66% of the sky with theleast foreground contamination the minimum detectable level of thetensor-to-scalar ratio would be about 0.002 at the 99% confidence level for anoptical depth of 0.1.Comment: 13 pages, 8 figures, replaced to match the accepted version in PR

Search for gravitational waves in the CMB after WMAP3: Foreground confusion and the optimal frequency coverage for foreground minimization