COSMOS2020: Cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to

We used the COSMOS2020 catalog to measure the stellar-to-halo mass relation (SHMR) divided by central and satellite galaxies from z = 0.2 to z = 5.5. Starting from accurate photometric redshifts, we measured the near-infrared selected two-point angular correlation and stellar mass functions in ten redshift bins. We used a phenomenological model that parametrizes the stellar-to-halo mass relation for central galaxies and the number of galaxies inside each halo to describe our observations. This model qualitatively reproduces our measurements and their dependence on the stellar mass threshold. Surprisingly, the mean halo occupation distribution only shows a mild evolution with redshift suggesting that galaxies occupy halos similarly throughout cosmic time. At each redshift, we measured the ratio of stellar mass to halo mass, M*/Mh, which shows the characteristic strong dependence of halo mass with a peak at $ M_h^{\rm peak} \sim 2 \times 10^{12} \, M_{\odot} $. For the first time, using a joint modeling of clustering and abundances, we measured the evolution of $ M_h^{\rm peak} $ from z = 0.2 to z = 5.5. $ M_h^{\rm peak} $ increases gradually with redshift from $ \log\,M_h^{\rm peak}/M_{\odot} \sim 12.1 $ at z ∼ 0.3 to $ \log\,M_h^{\rm peak}/M_{\odot} \sim 12.3 $ at z ∼ 2, and up to $ \log\,M_h^{\rm peak}/M_{\odot} \sim 12.9 $ at z ∼ 5. Similarly, the stellar mass peak $ M_{*}^{\rm peak} $ increases with redshift from $ \log\,M_*^{\rm peak}/M_{\odot} \sim 10.5 $ at z ∼ 0.3 to $ \log\,M_*^{\rm peak}/M_{\odot} \sim 10.9 $ at z ∼ 3. The SHMR ratio at the peak halo mass remains almost constant with redshift. These results are in accordance with the scenario in which the peak of star-formation efficiency moves toward more massive halos at higher redshifts. We also measured the fraction of satellites as a function of stellar mass and redshift. For all stellar mass thresholds, the satellite fraction decreases at higher redshifts. At a given redshift, there is a higher fraction of low-mass satellites and this fraction reaches a plateau at ∼25% at z ∼ 1. The satellite contribution to the total stellar mass budget in halos becomes more important than that of the central at halo masses of about Mh > 1013 M⊙ and always stays below the peak, indicating that quenching mechanisms are present in massive halos that keep the star-formation efficiency low. Finally, we compared our results with three hydrodynamical simulations: HORIZO