  We report high quality, Halpha or CO rotation curves (RCs) to several Re for
41 large, massive, star-forming disk galaxies (SFGs), across the peak of cosmic
galaxy evolution (z~0.67-2.45), taken with the ESO-VLT, the LBT and IRAM-NOEMA.
Most RC41 SFGs have reflection symmetric RCs plausibly described by equilibrium
dynamics. We fit the major axis position-velocity cuts with beam-convolved,
forward modeling with a bulge, a turbulent rotating disk, and a dark matter
(DM) halo. We include priors for stellar and molecular gas masses, optical
light effective radii and inclinations, and DM masses from abundance matching
scaling relations. Two-thirds or more of the z>1.2 SFGs are baryon dominated
within a few Re of typically 5.5 kpc, and have DM fractions less than maximal
disks (<fDM (Re)>=0.12). At lower redshift (z<1.2) that fraction is less than
one-third. DM fractions correlate inversely with the baryonic angular momentum
parameter, baryonic surface density and bulge mass. Inferred low DM fractions
cannot apply to the entire disk & halo but more plausibly reflect a flattened,
or cored, inner DM density distribution. The typical central 'DM deficit' in
these cores relative to NFW distributions is ~30% of the bulge mass. The
observations are consistent with rapid radial transport of baryons in the first
generation massive gas rich halos forming globally gravitationally unstable
disks, and leading to efficient build-up of massive bulges and central black
holes. A combination of heating due to dynamical friction and AGN feedback may
drive DM out of the initial cusps.
