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We use the COSMOS2020 catalogue 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 measure the near-infraredselected two-point angular correlation and stellar mass functions in tenredshift bins and fit them with an HOD-based model. At each redshift, wemeasure the ratio of stellar mass to halo mass, $M_*/M_h$, which shows thecharacteristic strong dependence of halo mass with a peak at $M_h^{\rm peak}\sim 10^{12}\, M_{\odot}$. Our results are in accordance with the scenario inwhich the peak of star-formation efficiency moves towards more massive halos athigher redshifts. We also measure the fraction of satellites as a function ofstellar mass and redshift. For all stellar mass thresholds the satellitefraction decreases at higher redshifts. At a given redshift there is a higherfraction of low-mass satellites. The satellite contribution to the totalstellar mass budget in halos becomes more important than centrals at halomasses of about $M_h > 10^{13} \, M_{\odot}$ and always stays below by peak,indicating that quenching mechanisms are present in massive halos that keep thestar-formation efficiency low. Finally, we compare our results with threehydrodynamical simulations Horizon-AGN, Illustris-TNG-100 and EAGLE. We findthat the most significant discrepancy is at the high mass end, where thesimulations generally show that satellites have a higher contribution to thetotal stellar mass budget than the observations. This, together with thefinding that the fraction of satellites is higher in the simulations, indicatesthat the feedback mechanisms acting in group-and cluster-scale halos appear tobe less efficient in quenching the mass assembly of satellites, and/or thatquenching occurs much later in the simulations.

COSMOS2020: The cosmic evolution of the stellar-to-halo mass relation for central and satellite galaxies up to z~5