Cosmological constraints from Subaru weak lensing cluster counts

We present results of weak lensing cluster counts obtained from 11-degree² Subaru/SuprimeCam data. Although the area is much smaller than previous work dealing with weak lensing peak statistics, the number density of galaxies usable for weak lensing analysis is about twice as large. The higher galaxy number density reduces the noise in the weak lensing mass maps, and thus increases the signal-to-noise ratio (S/N) of peaks of the lensing signal due to massive clusters. This enables us to construct a weak lensing selected cluster sample by adopting a high threshold S/N, such that the contamination rate due to false signals is small. We find six peaks with S/N > 5. For all the peaks, previously identified clusters of galaxies are matched within a separation of 1', demonstrating good correspondence between the peaks and clusters of galaxies. We evaluate the statistical error in the weak lensing cluster counts using mock weak lensing data generated from full-sky ray-tracing simulations, and find N_peak = 6 ± 3.1 in an effective area of 9.0 degree². We compare the measured weak lensing cluster counts with the theoretical model prediction based on halo models and place the constraint on the Ω_m-σ₈ plane which is found to be consistent with currently standard ΛCDM models. It is demonstrated that the weak lensing cluster counts can place a unique constraint on the σ₈-c₀ plane, where c₀ is the normalization of the dark matter halo mass-concentration relationship. Finally we discuss prospects for ongoing/future wide field optical galaxy surveys.