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We present a method for reducing cosmological data to constraints on theamplitudes of modes of the dark energy density as a function of redshift. Themodes are chosen so that (1) one of them has constant density and (2) theothers are non-zero only if there is time-variation in the dark energy densityand (3) the amplitude errors for the time-varying modes are uncorrelated witheach other. We apply our method to various combinations of three-year WMAPdata, baryon acoustic oscillation data, the 'Gold' supernova data set, and theSupernova Legacy Survey data set. We find no significant evidence for atime-varying dark energy density or for non-zero mean curvature. Although bysome measure the limits on four of the time-varying mode amplitudes are quitetight, they are consistent with the expectation that the dark energy densitydoes not vary on timescales shorter than a Hubble time. Since we do not expectdetectable time variation in these modes, our results should be viewed as asystematic error test which the data have passed. We discuss a procedure toidentify modes with maximal signal-to-noise ratio.Comment: 13 pages, 12 figures; Version accepted for publication by JCAP;  Updated with three-year WMAP data; added discussion on systematic error  detectio

Reduction of cosmological data for the detection of time-varying dark energy density