WMAP 
Wilkinson Microwave Anisotropy ProbeProduct Name
Beam Maps
Mission
WMAP
Coord. System
Focal Plane coordinates
Projection Type
Rectilinear, pixelized at 2.4 arcminutes (0.04^{°})
Resolution
0.23^{°} 0.93^{°} (frequency dependent)
Description The main and nearsidelobe response of each of the 20 WMAP antenna feeds
has been mapped inflight using observations of Jupiter. The 9year release
comprises 17 Jupiter observing seasons:
For purposes of constructing beam maps, the data in the hybrid beam TOD archive are assigned to 2.4 arcminute bins on a coordinate grid centered on either the A or Bside focal plane axis. The beam response for each feed is computed from the average temperature in each bin. No correction has been made for the sideA vs. sideB input transmission imbalance. These beam maps are convenient for some applications, but are not used in the computation of the flight beam transfer functions. The 2.4 arcminute binning acts as a smoothing kernel which filters high frequency spatial content. The pixelization transfer function may be estimated from the Legendre transform of the symmetrized radial profile of the binning kernel. Assuming a square pixel of 0.04 degrees on a side centered on the origin, the symmetrized radial profile of the binning function may be represented as
Beam maps are provided in 10 FITS image format files, one file for each differencing assembly. Each file contains:
The beam coordinates form an equal area rectangular coordinate system centered on the optic axis of the spacecraft. They are related to coordinates theta (elevation from optic axis) and phi (azimuth about optic axis) as follows:
The "optic axis" of the spacecraft is elevated by 19.5 degrees from the S/C XY plane and lies within the S/C YZ plane. Although this vector is close to the S/C Y axis (+ or  depending on A or B side), it becomes the Z axis of the focal plane coordinate system. For each differencing assembly, an azimuthally symmetrized radial beam profile is computed by binning the ensemble of individual A and B side hybridized Jupiter observations. A constant bin size of 0.25 arcmin is used, and the straight mean of all hybrid samples within a radial bin represents the value for that bin. Beam transfer functions are computed from the Legendre transform of the binned hybrid 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 b_l (amplitude) normalized to 1.0 at l=1. A third column has been added for the 9year release, which contains the fractional 1sigma error, delta_b_l/b_l. The method by which the error is computed is described in Hill et al. 2009, ApJ 180, 246. Product Name
Beam Transfer Function Fractional Covariance Matrices
Mission
WMAP
Description The matrices are provided in FITS image format, as a separate file for each DA. This is a symmetric matrix whose rows and columns are implicitly indexed by ascending multipole moment; the range of l is 0 to l_{max}, where l_{max} corresponds to NAXIS1  1 and is DAdependent. Since b_{l} is normalized to 1.0 at l=1, B_{ll′} is zero for entries with this multipole value. The square root of the diagonal of the matrix is identical to the fractional 1σ error provided in the Beam Transfer Function product. The method by which the fractional covariance is determined is described in Hill et al. 2009, ApJ 180, 246. Additional Information
