Table 5.
Fisher forecasts for a Euclid-like nontomographic analysis.
Statistics | Individual |
Added γ-2PCF |
Gain over γ-2PCF |
||||||
---|---|---|---|---|---|---|---|---|---|
δσ8/σ8 | δΩm/Ωm | FoM | δσ8/σ8 | δΩm/Ωm | FoM | δσ8 | δΩm | FoM | |
2nd order statistics | |||||||||
γ-2PCF | 0.75% | 1.17% | 2.56 × 105 | − | − | − | − | − | − |
κ-2PCF | 1.13% | 1.88% | 1.40 × 105 | 0.71% | 1.10% | 2.74 × 105 | ×1.06 | ×1.07 | ×1.07 |
HOS (Gaussian) | |||||||||
κ-PDF | 0.42% | 0.70% | 4.96 × 105 | 0.37% | 0.60% | 7.36 × 105 | ×2.01 | ×1.95 | ×2.87 |
Peaks | 0.45% | 0.70% | 4.28 × 105 | 0.40% | 0.64% | 5.28 × 105 | ×1.87 | ×1.84 | ×2.06 |
MFs | 0.35% | 0.74% | 2.60 × 105 | 0.32% | 0.49% | 7.29 × 105 | ×2.37 | ×2.40 | ×2.85 |
BNs | 0.72% | 1.27% | 9.82 × 104 | 0.54% | 0.85% | 3.87 × 105 | ×1.38 | ×1.37 | ×1.51 |
Pers. BNs | 0.32% | 0.60% | 6.95 × 105 | 0.29% | 0.53% | 8.29 × 105 | ×2.56 | ×2.23 | ×3.24 |
Pers. heat. | 0.56% | 0.86% | 3.44 × 105 | 0.45% | 0.72% | 4.98 × 105 | ×1.66 | ×1.63 | ×1.94 |
ST | 0.39% | 0.63% | 4.95 × 105 | 0.33% | 0.55% | 7.19 × 105 | ×2.30 | ×2.13 | ×2.81 |
All HOS | 0.16% | 0.27% | 4.96 × 106 | 0.16% | 0.26% | 5.03 × 106 | ×4.82 | ×4.41 | ×19.65 |
HOS (non-Gaussian) | |||||||||
HOM | 0.25% | 0.65% | 6.12 × 105 | 0.20% | 0.42% | 1.12 × 106 | ×3.72 | ×2.76 | ×4.37 |
![]() |
0.73% | 1.56% | 2.50 × 105 | 0.24% | 0.45% | 8.98 × 105 | ×3.17 | ×2.59 | ×3.51 |
![]() |
0.14% | 0.27% | 2.13 × 106 | 0.14% | 0.27% | 2.19 × 106 | ×5.49 | ×4.40 | ×8.55 |
Notes. The precision on σ8 and Ωm is given as a percentage of the fiducial values for the probes taken individually and when combined with the γ-2PCF. We also report the figure of merit (FoM) as defined in the Dark Energy Task Force (Albrecht et al. 2006). The last columns display the expected gain over the γ-2PCF analysis for the scales available in the DUSTGRAIN-pathfinder simulations. Results for non-Gaussian statistics are also presented as part of the HOWLS project; we stress, however, that a non-Gaussian likelihood would be necessary to assess the robustness of these three probes.
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