The formation and evolution of galaxies is closely connected to the dark matter halos they evolve in, and to the interaction between the baryons and the dark matter. For rotating spiral galaxies, the measure of rotation of the galaxy can be used to infer the underlying mass decomposition. We use high-resolution observations of 100 galaxies at z=0.6-2.5 taken mostly with VLT/SINFONI and KMOS (and some with NOEMA and ALMA), resolving the individual rotation curves up to more than twice the disk effective radius, where the gravitational effect of dark matter is important. We model each galaxy as a three component system with a Disk, bulge, and DM halo, and create a mock-observed rotating curve which we then fit to the data. We find that at higher redshifts, galaxies become more baryon dominated on average, although they exhibit a large scatter. Some galaxies require large amounts of dark matter, while the majority have little or close to no dark matter at all on the scale of the galaxy. We interpret these result in terms of the "deficit" in DM compared to cosmological scaling relations and the formation of a "core" in the halo density profile (rho~r^alhpa, where alpha=0), and show it is correlated with the rapid formation of a massive bulge in the center of these galaxies. Analytic models suggest strong AGN-driven feedback processes are a possible mechanism in the formation of these DM cores.