Wilkinson Microwave Anisotropy Probe DR2The data made available through this page has been updated. The most recent version of this data may be accessed through https://lambda.gsfc.nasa.gov/product/wmap/current/ Low Resolution Sky MapsCoordinate System:
Galactic
Projection Type:
0.23^{°} 0.93^{°} (frequency dependent)
Resolution:
HEALPix, nested, res 4 (Nside=16)
Download Links:
The low resolution (res 4) maps were used to study the influence of foregrounds on the polarization component of the WMAP data outside the Galactic plane. A map for each differencing assembly and each year of data was produced by degrading the normal resolution (res9) maps to res 4. The res 9 processing mask was used to block out the Galactic plane, resulting in a set of 85 res 4 pixels that were completely unpopulated. These pixels were repopulated from the res 9 data. The reason for this twostep procedure was to assure that data omitted by the processing mask at res 9 were excluded from the small subset of res 4 pixels that overlap the boundary of the cut. This processing resulted in 30 maps (3 years times 10 D/A's). The singleyear, singleD/A maps were combined into one map for each frequency band using a weighted average. There are 5 such maps, each comprising three years of data. In this case, the res 4 Galactic plane remains unpopulated for the Stokes I and spurious (S) components, because of zeropoint effects. Both the singleyear, singleD/A maps and the threeyear bandaveraged maps are available for download. The spurious signal (S) is not a Stokes parameter, but rather, an apparent signal generated by differences in the two radiometers that compose a differencing assembly. This component is computed by the mapmaking process, as discussed in Jarosik, et.al., 2006. The Stokes I and spurious (S) components included in the lowresolution map set are not suitable for direct use in analysis because of signal aliasing. Instead, their purpose is to help furnish a complete description of Stokes Q and U. 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
are:
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 = σ_{0} / sqrt(N_Obs)
where
Some files that contain polarization maps contain a second FITS extension
containing the #nxn# polarization noise covariance matrices for the pixels in the
maps of the first FITS extension. These matrices are used in the mapmaking
process and characterize the noise properties of the polarization maps. See
section 3.4 of Jarosik, et.al., 2006 in
the set of three year WMAP papers for more details. The columns of this extension are:
The covariance matrix of a pixel may be constructed by assembling the row elements into a 3x3 or 2x2 symmetric matrix with the form:
The size of the matrix depends upon whether or not the spurious signal component is included. The noise covariance matrices described above do not fully characterize the pixeltopixel noise in the res 4 maps. Therefore a more accurate, and much larger, inverse covariance matrix is supplied for each map as a separate product. This matrix consists of 12288x12288 elements in sixteen 3072x3072 blocks. The covariance matrices included in the map files comprise the diagonal elements of each of the blocks describing Q, U, and S coupling. The elements corresponding to the Galatic plane pixels as defined by the processing mask were set to zero. Therefore, the matrices as supplied are singular. To make them nonsingular, the row and the column corresponding to each zero element of the diagonal need to be deleted. A small effect due to transmission imbalance between the A side and the B side of the instrument has been projected out of the inverse variance matrices as described in Section 3.5.1 of Jarosik et al. (2007). See Jarosik, et.al., 2006 and Page, et.al., 2006 for more information. Additional Information
