In Dark Energy Survey and Kilo-Degree Survey + Collaboration (2023) we present a joint cosmic shear analysis of the Dark Energy Survey (DES Y3) and the + Kilo-Degree Survey (KiDS-1000) in a collaborative + effort between the two survey teams. We use a Hybrid analysis pipeline, defined from a mock survey study quantifying the + impact of the different analysis choices originally adopted by each survey team. + +
Download the cosmological chains presented in the DES Y3 + KiDS-1000 joint analysis. + Information about the adopted model and settings are documented in the file headers and + summarised in Table 2 of Dark Energy Survey and Kilo-Degree Survey + Collaboration (2023) + + When using the chains, the contribution of each sample must be weighted using the weight column. + The final N samples to be used are listed at the very end of the chain (nsample), along with the final log evidence. + Note that this chain used the Polychord nested sampler, so the sequence of samples is not a random walk.
+ +|
+ LCDM + |
+ File Name | +
|---|---|
|
+ Joint DES Y3 + KiDS-1000 cosmic shear + |
+
+ + + | +
|
+ Hybrid pipeline re-analysis of DES Y3 cosmic shear + |
+
+ + + | +
|
+ Hybrid pipeline re-analysis of KiDS-1000 cosmic shear + |
+
+ + + | +
We analyze the two-point functions using a pipeline developed in CosmoSIS. + The likelihood calculation for the combination of DES and KiDS can be accomplished using this file. + Note that due to minor updates in CosmoSIS, this calculation differs very slightly from the original version presented in + Dark Energy Survey and Kilo-Degree Survey + Collaboration (2023), but we have verified that there is no noticeable impact on the cosmological constraints.
+ +If you wish to analyse KiDS-1000 using correlated priors for the redshift nuisance parameters, + see this + CosmoSIS directory
+ + + +This fits table includes: the DES Y3 two-point correlation functions measured from a slightly reduced footprint to remove + areal overlap with KiDS-1000 (see Appendix A for details); the KiDS-1000 + COSEBIs E-modes; redshift distributions; analytical covariance matrices. Note that we assume DES Y3 and KiDS-1000 are independent. + There are the following 6 HDU extensions in the FITS binary file. +
+ +|
+ BinTableHDU 1 and 2: Name = nz_source_kids/nz_source_des +(Tomographic redshift distribution of the source galaxies) + |
+ ||
|---|---|---|
| + + Header Value + + | ++ Description + | +|
| NGAL_{i} | +
+ The mean number density (gal/arcmin^2) of the tomographic bin (1-5, KiDS) or (1-4, DES) + |
+ |
| SIG_E_{i} | +The total ellipticity dispersion of the tomographic bin (1-5, KiDS) or (1-4, DES) | +|
| + Column Name + | ++ Description + | +|
| Z_LOW | +The lower z boundary of this z bin range | +|
| Z_MID | +The central z of this z bin range + | +|
| Z_HIGH | +The upper z boundary of this z bin range + | +|
| BIN{i} | +The n(z) in this z bin range for tomographic bin (1-5, KiDS) or (1-4, DES) | +|
+
+
|
+ BinTableHDU 3: Name = En +(KiDS-1000 Cosmic shear En + COSEBIs) + |
+ ||
|---|---|---|
| + + Header Value + + | ++ Description + | +|
| KERNEL_1 | +
+ The HDU name of the corresponding first (source) redshift distribution + |
+ |
| KERNEL_2 | ++ The HDU name of the corresponding second (source) redshift distribution + | +|
| N_ZBIN_1 | +The number of first (source) tomographic bins + | +|
| N_ZBIN_2 | ++ The number of second + (source) tomographic bins + | +|
| N_ANG | +The number of COSEBIs modes | +|
| + Column Name + | ++ Description + | +|
| BIN1 | +Index of first (source) redshift bin | +|
| BIN2 | ++ Index of second (source) redshift bin + | +|
| ANGBIN | +Index of the COSEBIs mode | +|
| VALUE | ++ Measured value + | +|
| ANG | +Index of the COSEBIs mode | +|
+
+
|
+ BinTableHDU 4 and 5: Name = xip and xim +(Cosmic shear xi+/- + two-point shear correlation function) + |
+ ||
|---|---|---|
| + + Header Value + + | ++ Description + | +|
| KERNEL_1 | +
+ The HDU name of the corresponding first (source) redshift distribution + |
+ |
| KERNEL_2 | ++ The HDU name of the corresponding second (source) redshift distribution + | +|
| N_ZBIN_1 | +The number of first (source) tomographic bins + | +|
| N_ZBIN_2 | ++ The number of second + (source) tomographic bins + | +|
| N_ANG | +The number of angular bins | +|
| + Column Name + | ++ Description + | +|
| BIN1 | +Index of first (source) redshift bin | +|
| BIN2 | ++ Index of second (source) redshift bin + | +|
| ANGBIN | +Index of the angular bin | +|
| ANGMIN | +The lower angular bin edge [arcmin] | +|
| ANGMAX | +The upper angular bin edge [arcmin] | +|
| VALUE | ++ Measured value + | +|
| ANG | +Mean angular separation [arcmin] | +|
| NPAIRS | +Number of galaxy pairs in the bin | +|
+
+
|
+ ImageHDU = 1: Name = COVMAT +(Covariance matrix) + |
+ ||
|---|---|---|
| + Image HDU + | ++ Description + | +|
| Image array | +
+ 475x475 array of covariance matrix + |
+ |
| + Header Value + | ++ Description + | +|
| NAME_{i} (in header) | +The order of the covariance blocks (0-2), corresponding to the names of other HDUs that hold the data vector | +|
| STRT_{i} (in header) | +The start index of each covariance block (0-2) | +|
+
+
Release Notes:
+ +10 September 2023 : Joint re-analysis of DES Y3 and KiDS-1000 cosmic shear. Data vectors and chains in Y3KP DES+KiDS.
10 April 2023 : Release of Y3KP 6x2pt data vectors and chains in Y3KP+CMB lensing.
3 July 2022: Release of Y3KP extended cosmology likelihoods in Y3KP Beyond-L/wCDM.
3 March 2022: Release of Y3KP data vectors in Y3KP Products.
@@ -44,12 +46,13 @@5) Y3KP Catalogs: This section contains all catalogs used to run the main cosmological analysis from the cross-correlation of weak-lensing and clustering. It is serve as several h5 files, plus some code snippet (python) to interface with the data and isntructions to reproduce the catalogs used in our analysis
6) Y3KP Products: Data vectors and likelihoods from the main DES cosmological analysis (3x2pt statistics), combining weak lensing and galaxy clustering. These results used the Y3KP Catalogs described above.
7) Y3KP Beyond-L/wCDM: Likelihoods from DES Y3 3x2pt Extensions KP analysis (3x2pt statistics). These results used the Y3KP Catalogs described above.
-7) Y3KP+CMB lensing: Likelihoods from DES Y3 analysis including CMB lensing (6x2pt statistics). These results used the Y3KP Catalogs described above.
-8) BAO Sample: a subset of Gold products aimed at measuring the BAO scale; includes the catalogs, data vectors and likelihoods. The selection was based on the Y3 Gold catalog.
-9) redMaGiC Catalogs: Y3 redMaGiC galaxy catalogs
-10) WL Mass Maps: Mass maps reconstructed from weak lensing signal
-11) X-ray Clusters: X-ray selected galaxy clusters
-12) Galaxy Morphology: A Neural Network galaxy morphology catalog +
8) Y3KP+CMB lensing: Likelihoods from DES Y3 analysis including CMB lensing (6x2pt statistics). These results used the Y3KP Catalogs described above.
+9) BAO Sample: a subset of Gold products aimed at measuring the BAO scale; includes the catalogs, data vectors and likelihoods. The selection was based on the Y3 Gold catalog.
+10) redMaGiC Catalogs: Y3 redMaGiC galaxy catalogs
+11) WL Mass Maps: Mass maps reconstructed from weak lensing signal
+12) X-ray Clusters: X-ray selected galaxy clusters
+13) Galaxy Morphology: A Neural Network galaxy morphology catalog
+14) DES Y3 + KiDS-1000: A joint cosmic shear re-analysis
diff --git a/static/des_components/elements.html b/static/des_components/elements.html index 8830a7d..53ea2c0 100644 --- a/static/des_components/elements.html +++ b/static/des_components/elements.html @@ -118,6 +118,7 @@ +