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Window functions appropriate to each of the ten WMAP differencing assemblies have been derived in-flight from the calibrated time-ordered observations of Jupiter. For each differencing assembly, a symmetrized radial beam profile is computed by fitting the ensemble of individual A- and B-side Jupiter observations with Hermite polynomials of even order. The beam transfer function is then computed from the Legendre transform of the fit to the radial beam profile. The window function applicable to power spectra is the square of the beam transfer function.

Beam transfer functions are presented as ASCII tables, with the first column being multipole moment l and the second column the transfer function (amplitude) normalized to 1.0 at l=1.

More details can be found in:

"First Year Wilkinson Microwave Anisotropy Probe (WMAP) Results:
Beam Profiles and Window Functions", Page, et al...

"First Year Wilkinson Microwave Anisotropy Probe (WMAP) Results:
Angular Power Spectrum", Hinshaw et al 2003

WMAP Explanatory Supplement

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