Table 5.
Validation tests and resulting S8 marginal credible intervals.
| ID | Setup | M-HPD | PJ-HPD |
|---|---|---|---|
| 1 | 3 × 2 pt, reference | 0.037 | 0.038 |
| 2 | 3 × 2 pt, no GGL overlap | 0.037 | 0.038 |
| 3 | 3 × 2 pt, fiducial | 0.037 | 0.037 |
| 4 | CS+GGL, reference | 0.056 | 0.062 |
| 5 | CS+GC, reference | 0.036 | 0.039 |
| 6 | GGL+GC, reference | 0.079 | 0.108 |
| 7 | CS, reference | 0.061 | 0.061 |
| 8 | GC, reference | 0.090 | 0.111 |
| 9 | CS+GGL, analytic, Buceros | 0.054 | 0.072 |
| 10 | CS+GGL, analytic, Egretta | 0.056 | 0.062 |
| 11 | CS+GGL, mocks, Buceros | 0.054 | 0.057 |
| 12 | CS+GGL, mocks, Egretta | 0.057 | 0.066 |
| 13 | CS+GGL, S8 prior, corr δz | 0.056 | 0.062 |
| 14 | CS+GGL, S8 prior, uncorr δz | 0.057 | 0.074 |
| 15 | CS+GGL, lnAs prior, corr δz | 0.047 | 0.054 |
| 16 | CS+GGL, lnAs prior, uncorr δz | 0.045 | 0.047 |
Notes. Setups correspond to those shown in Fig. 22. The reference includes a more progressive selection of scales in the GGL data vector (Bands 1−7) than our fiducial analysis. GC corresponds to galaxy clustering, CS to cosmic shear, and ‘3 × 2 pt’ to the combination of all probes. Analytic/mocks and Buceros/Egretta indicates analytic and simulated covariances with simple or more realistic survey and sample properties. The choice of an (un)correlated prior on the source redshift distribution shifts is labelled as (un)corr δz. GGL signals with strong overlap of the lens and source redshift distributions have been removed in the ‘no GGL overlap’ case. We note that setup 4 is identical to 13. The two rightmost columns give the width of the 1σ credible intervals (CI) for the standard M-HPD credible interval and the PJ-HPD method, i.e. twice the standard deviation if the posterior was Gaussian.
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