Cosmological constraints from Subaru weak lensing cluster counts
  We present results of weak lensing cluster counts obtained from 11 sq.deg
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 as those. The higher galaxy
number density reduces the noise in the weak lensing mass maps, and thus
increases the signal-to-noise ratio 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 6 peaks with S/N>5. For all the peaks,
previously identified clusters of galaxies are matched within a separation of 1
arcmin, demonstrating good correspondence between the peaks and clusters of
galaxies. We evaluate the statistical error using mock weak lensing data, and
find Npeak=6+/-3.1 in an effective area of 9.0 sq.deg. We compare the measured
weak lensing cluster counts with the theoretical model prediction based on halo
models and place the constraint on Omega_m-sigma_8 plane which is found to be
consistent with currently standard LCDM models. It is demonstrated that the
weak lensing cluster counts can place a unique constraint on sigma_8-c_0 plane,
where c_0 is the normalization of the dark matter halo mass-concentration
relationship. Finally we discuss prospects for ongoing/future wide field
optical galaxy surveys.
