Cosmological constraints with weak lensing peak counts and second-order statistics in a large-field survey
Peak statistics in weak lensing maps access the non-Gaussian information contained in the large-scale distribution of matter in the Universe. They are therefore a promising complement to two-point and higher-order statistics to constrain our cosmological models. To prepare for the high-precision data of next-generation surveys, we assess the constraining power of peak counts in a simulated Euclid-like survey on the cosmological parameters $Ω_\mathrm{m}$, $σ_8$, and $w_0^\mathrm{de}$. In particular, we study how the Camelus model--a fast stochastic algorithm for predicting peaks--can be applied to such large surveys. We measure the peak count abundance in a mock shear catalogue of ~5,000 sq. deg. using a multiscale mass map filtering technique. We then constrain the parameters of the mock survey using Camelus combined with approximate Bayesian computation (ABC). We find that peak statistics yield a tight but significantly biased constraint in the $σ_8$-$Ω_\mathrm{m}$ plane, indicating the need to better understand and control the model's systematics. We calibrate the model to remove the bias and compare results to those from the two-point correlation functions (2PCF) measured on the same field. In this case, we find the derived parameter $Σ_8=σ_8(Ω_\mathrm{m}/0.27)^α=0.76_{-0.03}^{+0.02}$ with $α=0.65$ for peaks, while for 2PCF the value is $Σ_8=0.76_{-0.01}^{+0.02}$ with $α=0.70$. We therefore see comparable constraining power between the two probes, and the offset of their $σ_8$-$Ω_\mathrm{m}$ degeneracy directions suggests that a combined analysis would yield tighter constraints than either measure alone. As expected, $w_0^\mathrm{de}$ cannot be well constrained without a tomographic analysis, but its degeneracy directions with the other two varied parameters are still clear for both peaks and 2PCF. (abridged)