Uncorrelated Measurements of the Cmb Power Spectrum

will be uncorrelated, since 〈ĉĉ〉 − 〈ĉ〉〈ĉ〉 = I. 〈ĉ〉 = Mc, so the new window function matrix will be M. However, whereas the window functions of the original power estimates (the rows of F) are always well-behaved (they are always non-negative, and are generally quite narrow, as shown in the top panel of Figure 1), there is no guarantee that the same will hold for the new window functions. As was recently shown , however, one generally obtains beautiful window functions if one requires M to be lower-triangular, in which case F = MM corresponds to a Cholesky decomposition. For the COBE/DMR case aHubble Fellow