Table 4.
Improvement in the constraints for GCph alone, including magnification.
| Model | Ωm, 0 | Ωb, 0 | w0 | wa | h | ns | σ8 | ∑mν |
|---|---|---|---|---|---|---|---|---|
| ΛCDM | 21% | 0.3% | – | – | 1% | 12% | 28% | – |
| ΛCDM + ∑mν | 11% | 0.5% | – | – | 1.65% | 13% | 16% | 3% |
| w0 waCDM | 36% | 24% | 34% | 35% | 14% | 32% | 18% | – |
| w0 waCDM + ∑mν | 37% | 25% | 35% | 35% | 15% | 30% | 15% | 4% |
Notes. Shown is the improvement in the constraints (given by 1 − σmagn/σdens, in %), including magnification. We report the results for the same models as in Table 3, and, in the same way, we marginalise over the galaxy bias parameters. The values of the local count slope are fixed, and thus we assume a perfect knowledge of s(z) in each redshift bin.
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