Open Access

Fig. 7.


Lensing observational status. M500z plane with symbol colours representing the depth of the archival or dedicated lensing data. Shallow surveys like CFIS (and more so, DES, KiDS) yielding a density of background sources n ≲ 10 arcmin−2 cannot probe the low mass end of Tier-1 clusters with S/N > 3. Stacking of the shear signal will be unavoidable for these. Deep Subaru data enable such measurements on individual clusters since most observations reach source densities ≳20 arcmin−2. Euclid, which will reach n ≃ 30 arcmin−2 will greatly simplify cluster mass calibrations with lensing.

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