The connection between massive galaxies and their dark matter haloes from $z=0.25$ to $z\sim 4$ from the combined COSMOS, XMM-LSS and ECDF-S fields

Understanding how galaxies populate and grow within dark matter haloes is essential for linking the observed evolution of galaxies to the hierarchical growth of structure. We present a galaxy clustering analysis using optical and near-infrared data from the UltraVISTA and VIDEO surveys covering $9.3$ deg${}^2$ across the COSMOS, XMM-LSS and ECDF-S fields, $\sim 5\times$ larger than previous comparable studies, providing sufficient volume to determine the halo occupation of the most massive galaxies to $z\sim 4$. We measure the angular two-point correlation function for stellar-mass-selected galaxies over $0.25<z<4$ and by combining the three fields, we reduce the cosmic variance by a factor of $\sim 2$ compared to the individual fields. The stellar-to-halo mass ratio peaks at a halo mass of $M_h\approx {10}^{12}{\mathrm{M}}_{\odot }$ and is a maximum at $z\sim 1$. For the most massive galaxies, the peak halo mass ($M_h^{\mathrm{p}\mathrm{e}\mathrm{a}\mathrm{k}}$) increases from $z=1\to 0$, while the peak stellar mass in such haloes remains approximately constant, indicating that at $z<1$ massive galaxy formation becomes less efficient. We also find a steady increase in the satellite fraction since $z\sim 1$, from which we infer that massive halos continue to grow hierarchically while their central galaxies experience suppressed stellar-mass growth. We suggest this is due to the central massive galaxies having their growth controlled by feedback from active galactic nuclei feedback, likely from low-power stochastic radio emission.