These are the coadded maps of Q and U for Field A shown in the bottom two panels of Figure 4 in Kusaka et al. The HEALPix FITS file contains the following fields in order: More...
The ABS Field A mask excludes sources with flux density greater than 1000 mJy and applies a taper at the field edge boundary. This mask is applied to the maps before taking the power spectra.
This is the Hankel transform of the convolution of the beam and the pointing error (or jitter), effectively representing the effect of smearing of the map due to these effects. The first column is ℓ and the second column is the Legendre coefficient in the expansion. The square of the second column is the window function. The window function is shown in Figure 2 of Kusaka et al.
This file contains Stokes Q and U maps of the supernova remnant Taurus A in FITS format. There are three FITS HDUs, corresponding to the Q, U, and variance maps. More...
These 100 files contain realizations of the noise in the ABS maps. These realizations are generated using the observations that went into the final maps. In particular, they include pixel-to-pixel correlations and long timescale correlated, or so-called 1/f, noise.
