Wilkinson Microwave Anisotropy Probe
The data made available through this page has been updated. The most recent version of this data may be accessed through /product/map/current/
Sky Maps Per Frequency Band
HEALPix, nested, res 9 (Nside=512)
0.23°- 0.93° (frequency dependent)
Iterative algorithms are used to create skymaps from the calibrated differential time-ordered WMAP data for each of the ten differencing assemblies. Each pixel in a map represents a sky temperature for the bandpass appropriate to the differencing assembly. The CMB dipole has been removed from the Stokes I maps.
Maps for each year of WMAP data [currently the first, second, and third] were produced using the iterative method described above and have been supplied through LAMBDA. Full three year maps were produced by performing a weighted, pixel-by-pixel, mean of the three single year maps; the N_Obs measurement was used to weight this mean. The zero point of each three year Stokes I map has been set using a Galactic csc|b| model. The N_Obs measurements were added together to produce the final, three year, N_Obs measurement.
This same weighted mean method was then used to combine three year maps of the same frequency band into a single map for each frequency. Two maps were combined to produce the Q and V band maps; four maps were combined to produce the W band map.
WMAP maps are stored in FITS binary table extensions. The maps are stored in the first extension in a file; the format of this table depends upon whether polarization maps have been included in the file. Some files also contain the polarization covariance matrices for the maps; if supplied these matrices are stored in a second binary table extension.
As previously stated, the first FITS extension contains the maps. These maps
are in a nested HEALPix format, with
each row representing a single pixel. There are either four or two columns
depending upon whether or not polarization maps are included; these columns
The column names were selected to be compatible with existing HEALPix software. The TEMPERATURE and N_OBS columns are the only columns that exist in files that do not contain polarization maps.
Pixel noise in units of mK can be evaluated from N_obs with the expression
σ = σ0 / sqrt(N_Obs)
These σ0's were computed by averaging together the per-DA numbers.