Table 4
Summary of possible systematic errors and their expected impact on the reconstruction of b(k) or r(k) for a WMAP9 cosmology and our galaxy samples.
| Origin | Error b(k) | Error r(k) |
|---|---|---|
| Intr. align. |Aia|≈ 2 | ≲5.0% | ≲5.0% |
| Fiducial cosmology and model of Pm(k;χ) | 2.8% (3.0%) | 0.4% (1.1%) |
| Lens pd(z); δσ = 5% | 2.5% | 2.2% (2.7%) |
| Lens pd(z); δz = 1% | 1.9% | 0.5% (1.4%) |
| Source ps(z); δz = 1% | 1.9% | 0.5% (1.0%) |
| Shear bias m = 1% | 1.0% | 0.0% |
| Shear bias c ≈ 10−3% | <1.0% | <1.0% |
| Source ps(z); δσ = 5% | 0.8% | 0.5% (0.3%) |
| Reduced shear | ≲0.5% | ≲0.5% |
| Sampling noise of p(z) | 0.4% (0.6%) | 0.4% (0.5%) |
Notes. Values in brackets are for the high-z samples (
), which are only shown if they differfrom the low-z values (
). Sources have a mean redshift of 
. By δz and δσ we denote the relative error in the mean redshift and the redshift dispersion, respectively, which refer to either the lens redshift distribution, pd (z), or that of the sources, ps (z). We assume a constant residual shear bias m here.
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