The tarball vUitert18_KiDS450_data.tar.gz contains the following elements:
* full data vector (i.e. all band power spectra), with all corrections applied
The data vector is in the file Pkids_data_full_ibc2.dat.
The data is ordered as follows:
--- P^E ---
row 1: P^E S1 x S1 ell1
row 2: P^E S1 x S1 ell2
...
row 5: P^E S1 x S1 ell5
row 6: P^E S1 x S2 ell1
row 7: P^E S1 x S2 ell2
...
row 11: P^E S1 x S3 ell1
...
row 21: P^E S2 x S2 ell1
...
row 49: P^E S4 x S4 ell4
row 50: P^E S4 x S4 ell5
--- P^gm ---
row 51: P^gm F1 x S1 ell1
...
row 56: P^gm F1 x S2 ell1
...
row 89: P^gm F2 x S4 ell4
row 90: P^gm F2 x S4 ell5
--- P^gg ---
row 91: P^gg F1 x F1 ell1
...
row 100: P^gg F2 x F2 ell5
The notation follows the paper, i.e.
P^E -> cosmic shear (E-mode)
P^gm -> galaxy-galaxy lensing
P^gg -> angular clustering
[F1,F2] are the two foreground bins (GAMA); [S1, ..., S4] are the four background bins (KiDS).
[ell1,ell2,ell3,ell4,ell5] are the logarithmic means of the angular frequency bins, which have the values [200, 331, 548, 906, 1500].
Note that the power spectra are in the format P x ell^2 / 2 Pi (as in the plots).
* full covariance
The analytical covariance matrix is in Pkidscov_data_PlanckIter2.dat, with the first and second column indicating the elements (=row number in Pkids_data_full_ibc2.dat) and the third column the value of the covariance. It is the final covariance used after iteration (see the paper for details).
The covariance matrix is in the appropriate format for the data vector, i.e. for entries P x ell^2 / 2 Pi.
* redshift distributions
Histograms of the foreground distributions (GAMA) are in the files nz_GAMAz[1,2].dat.
Histograms of the background distributions (KiDS) are in the files nz_z[1-4]_kids_binned.dat.
In all cases the first column indicates the central redshift of a bin, and the second column the histogram value.