Multiresolution angular momentum measurements of z~1.5-2 star-forming
  galaxies
  We present detailed stellar specific angular momentum ($j_*$) measurements of
ten star-forming galaxies at $z\sim1.5-2$ using both high and low spatial
resolution integral field spectroscopic data. We developed a code that
simultaneously models the adaptive optics (AO) assisted observations from
OSIRIS/SINFONI along with their natural seeing (NS) counterparts from KMOS at
spatial resolutions of [$0.1-0.4$] arcsec and [$0.6-1.0$] arcsec respectively.
The AO data reveals 2/10 systems to be mergers and for the remaining eight the
mean uncertainties $\bar \Delta j_*$ decrease from 49% (NS), and 26.5% (AO), to
16% in the combined analysis. These $j_*$ measurements agree within 20% with
simple estimates ($\tilde{j_*}$) calculated from the Hubble Space Telescope
photometry and NS kinematics, however higher resolution kinematics are required
to first identify these disks. We find that the choice of surface mass density
model and the measurement of effective radius from photometry are the key
sources of systematic effects in the measurement of $j_*$ between different
analyses. Fitting the $j_*$ vs $M_*$ relations (Fall, 1983) with a fixed
power-law slope of $\beta=2/3$, we find a zero-point consistent with prior NS
results at $z\geq1$ within $\sim 0.3$ dex. Finally, we find a $\sim 0.38$ dex
scatter about that relation that remains high despite the AO data so we
conclude it is intrinsic to galaxies at $z>1$. This compares to a scatter of
$\leq 0.2$ dex for disks at $z\simeq0$ pointing to a settling of the Fall
relation with cosmic time.
