  We analyze Ha or CO rotation curves (RCs) extending out to several galaxy
effective radii for 100 massive, large, star-forming disk galaxies (SFGs)
across the peak of cosmic galaxy star formation (z~0.6-2.5), more than doubling
the previous sample presented by Genzel et al. (2020) and Price et al. (2021).
The observations were taken with SINFONI and KMOS integral-field spectrographs
at ESO-VLT, LUCI at LBT, NOEMA at IRAM, and ALMA. We fit the major axis
kinematics with beam-convolved, forward models of turbulent rotating disks with
bulges embedded in dark matter (DM) halos, including the effects of pressure
support. The fraction of dark to total matter within the disk effective radius
($R_e ~ 5 kpc$), $f_DM (R_e)=V_{DM}^2 (R_e)/V_{circ}^2 (R_e)$, decreases with
redshift: At z~1 (z~2) the median DM fraction is $0.38\pm 0.23$ ($0.27\pm
0.18$), and a third (half) of all galaxies are "maximal" disks with $f_{DM}
(R_e)<0.28$. Dark matter fractions correlate inversely with the baryonic
surface density, and the low DM fractions require a flattened, or cored, inner
DM density distribution. At z~2 there is ~40% less dark matter mass on average
within $R_e$ compared to expected values based on cosmological stellar-mass
halo-mass relations. The DM deficit is more evident at high star formation rate
(SFR) surface densities ($\Sigma_{SFR}>2.5 M_{\odot} yr^{-1} kpc^{-2}$) and
galaxies with massive bulges ($M_{bulge}>10^{10} M_{\odot}$). A combination of
stellar or active galactic nucleus (AGN) feedback, and/or heating due to
dynamical friction, either from satellite accretion or clump migration, may
drive the DM from cuspy into cored mass distributions. The observations
plausibly indicate an efficient build-up of massive bulges and central black
holes at z~2 SFGs.
