Figure Data for "A Unified Photometric Redshift Calibration for Weak Lensing Surveys using the Dark Energy Spectroscopic Instrument"

Supplementary material to DESI's publication "A Unified Photometric Redshift Calibration for Weak Lensing Surveys using the Dark Energy Spectroscopic Instrument" to comply with the data management plan. In the following, we list the files associated with each figure. "title_{a,b}.csv" means that both "title_a.csv" and "title_b.csv" would belong to that figure. All the code used in the analysis is provided in code.zip. Figure 1: map.fits The map is stored as a table of coordinates, i.e., right ascension (column RA) and declination (column DEC) in degrees, indicating whether each point is within the survey. The different surveys are identified by their respective columns: the COSMOS2020 catalog is stored in the COSMOS2020 column, the Dark Energy Survey Y3 catalog in the DES column, the Hyper Suprime-Cam Y1 data set in the HSC column, and the Kilo-Degree Survey 1000-square degree release in the KIDS column. The DESI COSMOS footprint is approximated as a circle with 1.7 degree radius centered on RA = 150.80 deg and DEC = 2.20 deg. Figure 2: calibration_*.csv The results are stored in 4 separate files with descriptive filenames and column names, each corresponding to one of the 4 panels in this figure. Figure 3: som_{des,kids}.csv The results are stored in separate files for the DES and KiDS SOMs, corresponding to the upper and lower row of panels, respectively. Results are stored as tables with columns DATA (left two panels) and PREDICTION (middle two panels). The right two panels are the difference between them. Figure 4: verification.csv The upper panels, the weighted fractions of redshifts coming from DESI, can be re-created by plotting F_DESI_<SURVEY>_<BIN>, where <SURVEY> is the weak lensing survey (DES, HSC or KIDS) and <BIN> the tomographic bin (1 to 5), as a function of P_F_MIN, the threshold of the fiber probability. The lower panels are produced by taking the inverse square-root of the effective sample size, N_EFF_<SURVEY>_<BIN>. Figure 5: verification.csv Data for the upper pane showing the change in the mean COSMOS2020 redshift is given in the DELTA_Z_C20_<SURVEY>_<BIN> column. As for Figure 4, the data has to be plotted against the threshold on the fiber probability, P_F_MIN. Finally, the data for the lower panels of Figure 4 is stored in the SIGMA_DELTA_Z_C20_<SURVEY>_<BIN> columns. Figure 6: nz.csv The photometric redshift calibrations produced in this work are given in the <SURVEY>_<BIN>_<TYPE> columns. Here, <TYPE> denotes the redshift source, i.e., 1 for DESI-LSS, 2 for DESI-Other, 3 for DESI-Fail and 4 for COSMOS2020. The bins are defined by the minimum (A_MIN) and maximum scale factor (A_MAX). The fiducial redshift calibrations are publicly available and can be obtained from the individual survey collaborations. Figure 7: kids_cosmo_{this_work,fiducial}.fits The files contain the weighted posteriors for $\Omega_\mathrm{m}$ (column O_M) and $S_8$ (column S_8). Weights are stored in the column W and represent the absolute weight (not the natural logarithm). The posterior for the Planck CMB analysis is publicly available via the ESA website at https://wiki.cosmos.esa.int/planck-legacy-archive/index.php/Cosmological_Parameters. Figure 8: kids_transfer_som.fits The file contains a table with descriptive column names, i.e., KIDS WIDE for the data corresponding to the density depicted in the left panel. Figure 9: kids_transfer_magnitudes.fits The file contains a table. The r-band magnitudes are stored in the column R and the r-Z color in the column R-Z. The different densities are stored in the remaining columns with descriptive names.