KiDS/2dFLenS data release

Tarball Download:[link to data] 

This README contains the relevant information about the structure and ordering of the various data files. Please read Joudaki et al. (2018) for the details of the KiDS/2dFLenS analysis. This tarball contains:

1) Data vector (tomographic two-point correlation functions, redshift-space multipole power spectra)

2) Covariance matrix

3) Masking files

4) Redshift distributions (with 1000 bootstrap realizations for error analyses)

5) Convolution matrices

Acknowledgements:

Users of these data should include an acknowledgement to: 

Joudaki et al. (2018), arXiv:1707.06627 [KiDS x (2dFLenS + BOSS)]
Hildebrandt et al. (2017), arXiv:1606.05338 [KiDS-450]
Blake et al. (2016), arXiv:1608.02668 [2dFLenS]
Anderson et al. (2014), arXiv:1312.4877 [BOSS DR10]

If using our lensing/RSD code (CosmoLSS), please also acknowledge:

Joudaki et al. (2017a), arXiv:1601.05786
Joudaki et al. (2017b), arXiv:1610.04606
Joudaki et al. (2018), arXiv:1707.06627

If using HMCODE (as part of CosmoLSS), please also acknowledge:

Mead et al. (2015), arXiv:1505.07833
Mead et al. (2016), arXiv:1602.02154

The contents of the data release

Both 2dFLenS and BOSS are restricted to the overlapping areas with KiDS-450, and divided into `low-redshift' and `high-redshift' galaxy samples, covering $0.15 < z < 0.43$ (2dFLOZ, LOWZ) and $0.43 < z < 0.70$ (2dFHIZ, CMASS). The full 2dFLenS data release is found here.

1) Data vector

DATA_VECTOR.dat files contain 4 columns: ibin, xi, JK error, sim error. Only the xi column is used by the CosmoLSS likelihood code (together with covariance matrix below).

The file "xipmcut_kids_regcomb_blind2_swinburnesj.dat" contains the KiDS 2pt shear correlation function measurements used together with the numerical covariance (the file "xipmcut_kids_blind1.dat" is used with the analytic covariance matrix). Given 4 tomographic bins and 9 angular bins, there are 180 elements pre-masking, and 130 elements post-masking. The format follows the convention of Heymans et al (2013), such that for each unique pair of tomographic bins, the \xi_+ values are listed with increasing angular scale, followed by the \xi_- values. The pairs of tomographic bins ij are then ordered as (11, 12, 13, 14, 22, 23, 24, 33, 34, 44). For each of the 4 tomographic bins, our measurements are evaluated at [0.7134, 1.452, 2.956, 6.017, 12.25, 24.93, 50.75, 103.3, 210.3] arcmin.

The file "xipmcut_kids_blind1_planckcut.dat" is restricted to the data used in the "large-scale" (linear) cosmic shear analysis (with analytical covariance). This includes only the data points evaluated at [24.93, 50.75] arcmin for xi_+ and 210.3 arcmin for xi_-.

The file "xipmgtpllarge4_kids_regcomb_blind2sj.dat" contains the full lensing/RSD data vector (post-masking). There are 130 elements from cosmic shear, 64 elements from galaxy-galaxy lensing, and 16 elements from the multipole power spectra (monopole P_0 and quadrupole P_2; the hexadecapole P_4 is masked out). The galaxy-galaxy lensing measurements are evaluated at [12.25, 24.93, 50.75, 103.3] arcmin, and the multipole power spectra are evaluated at k = [0.075, 0.125] h/Mpc. The first 130 elements follow the same structure as cosmic shear alone (above). The following 64 galaxy-galaxy lensing data points are structured in 4 sets of 16 elements, such that the each set corresponds to a given cross-correlation (KiDS x 2dFLOZ, KiDS x 2dFHIZ, KiDS x CMASS, KiDS x LOWZ --- in that order). Each set of 16 elements corresponds to KiDS tomographic bin i (=1,2,3,4) correlated with the given spectroscopic sample, i.e. KiDS tomographic bin1 x 2dFLOZ for angular bin at 12.25 arcmin, followed by the cross-correlation at 24.93 arcmin, and so on, then KiDS tomographic bin2 x 2dFLOZ at 12.25 arcmin, followed by the cross-correlation at 24.93 arcmin, and so on. This structure is naturally adhered to by the likelihood code. The last 16 elements are given by the multipole power spectra, structured in four sets of 4 elements, such that each set corresponds to 2dFLOZ, 2dFHIZ, CMASS, LOWZ (in that order). Each set of 4 elements are given by [P_0(k_1), P_0(k_2), P_2(k_1), P_2(k_2)], where k_1 = 0.075 h/Mpc, and k_2 = 0.125 h/Mpc.

The file "xipmgtpllarge7_kids_regcomb_blind2sj.dat" contains the full lensing/RSD data vector (post-masking) for conservative data cuts. There are 130 elements from cosmic shear, 48 elements from galaxy-galaxy lensing, and 8 elements from the multipole power spectra. The galaxy-galaxy lensing measurements are evaluated at [24.93, 50.75, 103.3] arcmin, and the multipole power spectra are evaluated at k = 0.075 h/Mpc.

The file "xipmgtlarge4_kids_regcomb_blind2sj.dat" is the same as "xipmgtpllarge4_kids_regcomb_blind2sj.dat" except it does not contain multipole power spectrum measurements (i.e. only cosmic shear + galaxy-galaxy lensing).

The file "xipmgtlarge3_kids_regcomb_blind2sj.dat" is the same as "xipmgtpllarge7_kids_regcomb_blind2sj.dat" except it does not contain multipole power spectrum measurements (i.e. only cosmic shear + galaxy-galaxy lensing).

2) Covariance matrix

All covariance matrices also have the same file names as the data vectors above with the addition of the letters "cov". The 3 columns are: ibin, jbin, Cov(ibin,jbin) where ibin/jbin follow the same structure as the data vector files.

3) Masking files

All masking files also have the same file names as the data vectors above with the addition of the letters "select". The 2 columns are: ibin, iselect. When iselect = 0 the data point is removed from the likelihood analysis (i.e. these files are necessary for matching the theory vectors to the data vectors in the likelihood calculation).

4) Redshift distributions

The files "hendriknz/nz_zi_kids_bootj.dat" contain the KiDS-450 source redshift distributions for each tomographic bin i and bootstrap realization j, with format z n(z), where i runs from 1 to 4 and j runs from 0 to 999. If use_bootstrapnz = F is set in CosmoLSS, the mean redshift distributions "nz_zi_kids_binned.dat" are used instead. We also provide the lens redshift distributions in "nz_LENS_modelsj.dat", with format z n(z), where "LENS" is given by [2dfloz, 2dfhiz, cmass, lowz].

5) Convolution matrices

The convolution matrices (in the Multipole_overlap directory) are needed in the galaxy clustering analysis (see equation 17 in Joudaki et al. 2018). As we consider 10 k values for P_0, P_2, P_4, there are four 30 x 30 matrices, one each for 2dFLOZ, 2dFHIZ, CMASS, LOWZ. The k values extend from 0 to 0.5 h/Mpc in steps of 0.05 h/Mpc. The format is: ibin, jbin, M(i,j), such that for ibin=1, the first 10 elements in jbin correspond to increasing values of k for P_0, the next 10 elements for P_2, and the last 10 elements for P_4, and so on (continuing to ibin=2). 

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If you have any questions or queries about this data release, please do not hesitate to contact Shahab Joudaki (shahab.joudaki@physics.ox.ac.uk)