The data made available through this page has been updated. The most recent version of this data may be accessed through /product/map/current/
Beam Transfer Functions
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: