Speaker
Description
Context. The spatial distribution of galaxy clusters provides a reliable tracer of the large-scale distribution of matter in the Universe.
The clustering signal depends on intrinsic cluster properties and cosmological parameters.
Aims. The ability of eROSITA on board Spectrum-Roentgen-Gamma (SRG) to discover galaxy clusters allows the association of
extended X-ray emission with dark matter haloes to be probed. We measured the projected two-point correlation function to study the
occupation of dark matter haloes by clusters and groups detected by the first eROSITA all-sky survey (eRASS1).
Methods. We created five volume-limited samples probing clusters with different redshifts and X-ray luminosity values. We inter-
preted the correlation function with halo occupation distribution (HOD) and halo abundance matching (HAM) models. We simulta-
neously fit the cosmological parameters and halo bias of a flux-limited sample of 6493 clusters with purity > 96%.
Results. We obtained a detailed view of the halo occupation for eRASS1 clusters. The fainter population at low redshift (S0: LX =
4.63 × 1043 erg/s, 0.1 < z < 0.2) is the least biased compared to dark matter, with b = 2.95 ± 0.21. The brightest clusters up to higher
redshift (S4: LX = 1.77 × 1044 erg/s , 0.1 < z < 0.6) exhibit a higher bias b = 4.34 ± 0.62. Satellite groups are rare, with a satellite
fraction < 14.9% (8.1) for the S0 (S4) sample. We combined the HOD prediction with a HAM procedure to constrain the scaling
relation between LX and mass in a new way, and find a scatter of ⟨σLx ⟩ = 0.36. We obtain cosmological constraints for the physical
+1.02
cold dark matter density ωc = 0.12+0.03
−0.02 and an average halo bias b = 3.63−0.85 .
Conclusions. We modelled the clustering of galaxy clusters with a HOD approach for the first time, paving the way for future studies
combining eROSITA with 4MOST, SDSS, Euclid, Rubin, and DESI to unravel the cluster distribution in the Universe.
