The factor 10,000 ensures that we get weights of convenient size. This error or standard deviation may be computed from differences between consecutive, phased observations within a specified interval, such as 0.005p (or more in the maximum part of an EA-type light curve). The computed error will then be of the form

JAii )2

where p is the number of pairings, probably less than 2n, where n is the number of independent observations i because not all parts of the light curve may be equally well covered. Alternatively, a may be computed from the fit error of a truncated Fourier series representation of the light curve outside of the eclipse. This method is not without pitfalls, however. Perturbations may influence the light curve and cause higher-order terms in the Fourier series of the form

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