Rotation Curves in z~1-2 Star-Forming Disks: Comparison of Dark Matter
  Fractions and Disk Properties for Different Fitting Methods
  We present a follow-up analysis examining the dynamics and structures of 41
massive, large star-forming galaxies at z~0.67-2.45 using both ionized and
molecular gas kinematics. We fit the galaxy dynamics with models consisting of
a bulge, a thick, turbulent disk, and a NFW dark matter halo, using code that
fully forward models the kinematics, including all observational and
instrumental effects. We explore the parameter space using Markov Chain Monte
Carlo (MCMC) sampling, including priors based on stellar and gas masses and
disk sizes. We fit the full sample using extracted 1D kinematic profiles. For a
subset of 14 well-resolved galaxies, we also fit the 2D kinematics. The MCMC
approach robustly confirms the results from least-squares fitting presented in
Paper I (Genzel et al. 2020): the sample galaxies tend to be baryon-rich on
galactic scales (within one effective radius). The 1D and 2D MCMC results are
also in good agreement for the subset, demonstrating that much of the galaxy
dynamical information is captured along the major axis. The 2D kinematics are
more affected by the presence of non-circular motions, which we illustrate by
constructing a toy model with constant inflow for one galaxy that exhibits
residual signatures consistent with radial motions. This analysis, together
with results from Paper I and other studies, strengthens the finding that
massive, star-forming galaxies at z~1-2 are baryon-dominated on galactic
scales, with lower dark matter fractions towards higher baryonic surface
densities. Finally, we present details of the kinematic fitting code used in
this analysis.
