Weak lensing is a physical phenomenon which describes light deflection by gravity. Light rays emitted from distanced galaxies can be slightly perturbed, which distort the images of these galaxies. By measuring the distortion, cosmologists can study the matter distribution and improve our knowledge about the history and the composition of the Universe.
One simple way to study weak lensing is peak counts. Peaks are local maxima of the projected mass distribution. Therefore, they are direct tracers of massive structures, and are related to the mass function of the dark matter halo distribution. Peak statistics have already been shown as a powerful tool to constrain cosmological models.
Three advantages can be outlined from this model:
This new model has already showed its strong potential in mock analyses. We look forward to applying it to the real data.