Multi-scale weak lensing detection of galaxy clusters with source redshift tomography

A number of methods have emerged to detect galaxy clusters solely through their weak lensing signal. Using the recently introduced wavelet multi-scale detection method, here we focus on the potential of using tomographic information of source galaxies to increase the number of weak lensing detections. We applied the z s , min -cut technique, consisting of a combination of weak lensing peak detections emerging from lensing maps obtained using different source redshift bins, to mock datasets of progressively increasing sophistication. The source redshift distribution was chosen to be Euclid -like, with a maximum depth of z s , max = 3, and overlapping tomographic redshift bins were constructed by progressively increasing the minimum source redshift z s , min . Considering all possible detection combinations from one to four tomographic bins, we find that a single source redshift bin, with z s , min = 0.4, performs as well as the combination of multiple redshift bins. By running detections on synthetic clusters of varying complexity, from isolated Navarro Frenk White haloes to haloes embedded in and formed within N-body cosmological simulations, and considering both true and photometric source redshifts, we show that while large-scale structure contamination and photometric redshift errors reduce the potential gains of the tomographic approach, the dominant limitation is the accumulation of spurious detections across redshift bins, which lead to decreased purity at a fixed detection threshold.