We describe a class of observational strategies for probing the anisotropies in the cosmic microwave background (CMB) where the instrument scans on rings which can be combined into an n-torus, the ring torus. This class has the remarkable property that it allows exact maximum likelihood power spectrum estimation in of order N^2 operations (if the size of the data set is N) under circumstances which would previously have made this analysis intractable: correlated receiver noise, arbitrary

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... ric beam shapes and far side lobes, non-uniform distribution of integration time on the sky and partial sky coverage. This ease of computation gives us an important theoretical tool for understanding the impact of instrumental effects on CMB observables and hence for the design and analysis of the CMB observations of the future. There are members of this class which closely approximate the MAP and Planck satellite missions. We present a numerical example where we apply our ring torus methods to a simulated data set from a CMB mission covering a 20 degree patch on the sky to compute the maximum likelihood estimate of the power spectrum C_ℓ with unprecedented efficiency.