The angular momentum distribution and baryon content of star forming
  galaxies at z~1-3
  We analyze the angular momenta of massive star forming galaxies (SFGs) at the
peak of the cosmic star formation epoch (z~0.8-2.6). Our sample of ~360
log(M*/Msun) ~ 9.3-11.8 SFGs is mainly based on the KMOS3D and SINS/zC-SINF
surveys of H$\alpha$ kinematics, and collectively provides a representative
subset of the massive star forming population. The inferred halo scale angular
momentum distribution is broadly consistent with that theoretically predicted
for their dark matter halos, in terms of mean spin parameter <$\lambda$> ~
0.037 and its dispersion ($\sigma_{log(\lambda)}$~0.2). Spin parameters
correlate with the disk radial scale, and with their stellar surface density,
but do not depend significantly on halo mass, stellar mass, or redshift. Our
data thus support the long-standing assumption that on average, even at high
redshifts, the specific angular momentum of disk galaxies reflects that of
their dark matter halos (j_d = j_DM). The lack of correlation between $\lambda$
x (j_d/j_DM) and the nuclear stellar density $\Sigma_{*}$(1kpc) favors a
scenario where disk-internal angular momentum redistribution leads to
"compaction" inside massive high-redshift disks. For our sample, the inferred
average stellar-to-dark matter mass ratio is ~2%, consistent with abundance
matching results. Including the molecular gas, the total baryonic disk-to-dark
matter mass ratio is ~5% for halos near $10^{12}$ Msun, which corresponds to
31% of the cosmologically available baryons, implying that high-redshift disks
are strongly baryon dominated.
