II. Apples to apples $A^2$: cluster selection functions for next-generation surveys

Abstract

We present the cluster selection function for three of the largest next-generation stage-IV surveys in the optical and infrared: Euclid-Optimistic, Euclid-Pessimistic and the Large Synoptic Survey Telescope (LSST). To simulate these surveys, we use the realistic mock catalogues introduced in the first paper of this series. We detected galaxy clusters using the Bayesian Cluster Finder (BCF) in the mock catalogues. We then modeled and calibrated the total cluster stellar mass observable-theoretical mass ($M_{\mathrm{CL}}^{\ast }-M_{\mathrm{h}}$) relation using a power law model, including a possible redshift evolution term. We find a moderate scatter of ${\sigma }_{M_{\mathrm{CL}}^{\ast }|M_{\mathrm{h}}}$ of 0.124, 0.135 and 0.136 $\mathrm{dex}$ for Euclid-Optimistic, Euclid-Pessimistic and LSST, respectively, comparable to other work over more limited ranges of redshift. Moreover, the three datasets are consistent with negligible evolution with redshift, in agreement with observational and simulation results in the literature. We find that Euclid-Optimistic will be able to detect clusters with $>80\%$ completeness and purity down to $8\times 10^{13}{h}^{-1}{M}_{\odot }$ up to $z<1$. At higher redshifts, the same completeness and purity are obtained with the larger mass threshold of $2\times 10^{14}{h}^{-1}{M}_{\odot }$ up to $z=2$. The Euclid-Pessimistic selection function has a similar shape with $\sim 10\%$ higher mass limit. LSST shows $\sim 5\%$ higher mass limit than Euclid-Optimistic up to $z<0.7$ and increases afterwards, reaching values of $2\times 10^{14}{h}^{-1}{M}_{\odot }$ at $z=1.4$. Similar selection functions with only $80\%$ completeness threshold have been also computed. The complementarity of these results with selection functions for surveys in other bands is discussed.

13 pages, 10 figures, accepted for publication in MNRAS

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