2020MNRAS.497.5220C

Protoclusters, which will yield galaxy clusters at lower redshift, can provide valuable information on the formation of galaxy clusters. However, identifying progenitors of galaxy clusters in observations is not an easy task, especially at high redshift. Different priors have been used to estimate the overdense regions that are thought to mark the locations of protoclusters. In this paper, we use mimicked Ly α-emitting galaxies at z = 5.7 to identify protoclusters in the MultiDark galaxies, which are populated by applying three different semi-analytic models to the 1 h^–1 Gpc MultiDark Planck2 simulation. To compare with observational results, we extend the criterion 1 (a Ly α luminosity limited sample) to criterion 2 (a match to the observed mean galaxy number density). To further statistically study the finding efficiency of this method, we enlarge the identified protocluster sample (criterion 3) to about 3500 at z = 5.7 and study their final mass distribution. The number of overdense regions and their selection probability depends on the semi-analytic models and strongly on the three selection criteria (partly by design). The protoclusters identified with criterion 1 are associated with a typical final cluster mass of 2.82±0.92 ×10¹⁵ M_☉, which is in agreement with the prediction (within ±1σ) of an observed massive protocluster at z = 5.7. Identifying more protoclusters allows us to investigate the efficiency of this method, which is more suitable for identifying the most massive clusters: completeness (C) drops rapidly with decreasing halo mass. We further find that it is hard to have a high purity (P) and completeness simultaneously.