Abstract
Cluster number count is a major cosmological probe for the next generation of cosmological large scale-structure surveys like the one expected from the Euclid satellite mission. Cosmological constraints will be mainly limited by the understanding of the selection function (SF), which characterize the probability of detecting a cluster of a given mass and redshift. The SF can be estimated by injecting realistic simulated clusters into the survey and re-applying the detection procedure. For this purpose we intend to use The Three Hundreds project, a 324 cluster sample simulated with full-physics hydrodynamical re-simulations. In this paper we concentrate on the study of the distribution of member galaxies in the cluster sample. First, we study possible resolution effects by comparing low and high resolution simulations. Finally, accounting for the latter we derive the density profiles of the member galaxies and discuss their evolution with cluster mass and redshift.
Highlights
The generation of large-scale structure survey instruments, like the Euclid satellite [1] and the Rubin observatory [2], will use cluster abundance as a major cosmological probe to constraint the parameters of the ΛCDM cosmological model
It is necessary to account for the probability of finding a cluster at a certain mass and redshift in this solid angle, which is known as the Selection Function (SF)
The Three Hundreds project consists of a 324 cluster sample simulated with full-physics hydrodynamical re-simulations
Summary
The generation of large-scale structure survey instruments, like the Euclid satellite [1] and the Rubin observatory [2], will use cluster abundance as a major cosmological probe to constraint the parameters of the ΛCDM cosmological model. In order to estimate the SF, it is needed to use simulated data sets. These can be either a full mock galaxy catalogue including clusters and field galaxies, or individual simulated clusters which are injected in the observed galaxy. A solution to this is the ‘zoom’ simulations, as adopted by The Three Hundreds [7] For this project, a large cosmological volume is simulated by Nbody dark-matter-only simulation, and only in the regions where a galaxy cluster is found, full-physics simulations are performed. We describe in this paper the main optical and IR properties of the Three Hundreds clusters in the prospect of using them for computing the SF of future cluster catalogues like the one expected for the Euclid satellite
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