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We present stellar specific angular momentum $j_*$ measurements of two $z\sim1.5$ galaxies in the KGES sample and 12 DYNAMO $z\sim 0.1$ analogues ofhigh-redshift galaxies. We combine natural seeing integral field spectroscopicdata to trace line emission out to high multiples of effective radius $r_e$,with adaptive optics assisted Keck/OSIRIS observations to trace the rapid risein rotation curve in the inner regions. Our spaxel-wise integration methodgives results that are on average within measurement uncertainty of thetraditional rotation curve model method. At $z\sim 0$, combining GMOS andOSIRIS datasets improves the measurement uncertainty in $j_*$ from 13\% (GMOSonly) or 16\% (OSIRIS only) to 10\%. At $z\sim 1.5$, systematics allow for atbest 20\% uncertainty on $j_*$. DYNAMO analogues of high-$z$ galaxies have low$j_*$ for their stellar mass $M_*$, and low bulge-to-total light ratio $\beta$for their $j_*/M_*$. The high-$z$ galaxy COSMOS 127977 has $j_*/M_*$ consistentwith normal local disk galaxies, while UDS 78317 is consistent with localanalogues. However, our high-resolution OSIRIS data reveal that UDS 78317 maybe a merging system. We report a relationship between distance to the$\beta-j_*/M_*$ plane and the ratio of velocity dispersion to rotationalvelocity $\sigma/v_{max}$, where galaxies that deviate more from the plane aremore dispersion-dominated due to turbulence. Much of the scatter in $M_*-j_*$that is not explained by variations in the bulge-to-total ratio or evolutionwith redshift may be driven by increased turbulence due to star formation, orby treating mergers as rotating disks.

Angular momentum of $z\sim 1.5$ galaxies and their local analogues with adaptive optics