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We present an analysis of the gas dynamics of star-forming galaxies at z~1.5using data from the KMOS Galaxy Evolution Survey (KGES). We quantify themorphology of the galaxies using $HST$ CANDELS imaging parametrically andnon-parametrically. We combine the H$\alpha$ dynamics from KMOS with thehigh-resolution imaging to derive the relation between stellar mass (M$_{*}$)and stellar specific angular momentum (j$_{*}$). We show that high-redshiftstar-forming galaxies at z~1.5 follow a power-law trend in specific stellarangular momentum with stellar mass similar to that of local late-type galaxiesof the form j$_*$$\propto$M$_*^{0.53 \pm 0.10}$. The highest specific angularmomentum galaxies are mostly disc-like, although generally, both peculiarmorphologies and disc-like systems are found across the sequence of specificangular momentum at a fixed stellar mass. We explore the scatter within thej$_{*}$-M$_{*}$ plane and its correlation with both the integrated dynamicalproperties of a galaxy (e.g. velocity dispersion, Toomre Q$_{\rm g}$, H$\alpha$star formation rate surface density $\Sigma_{\rm SFR}$) and its parameterisedrest-frame UV/optical morphology (e.g. S\'ersic index, bulge to total ratio,Clumpiness, Asymmetry and Concentration). We establish that the position in thej$_{*}$-M$_{*}$ plane is strongly correlated with the star-formation surfacedensity and the Clumpiness of the stellar light distribution. Galaxies withpeculiar rest-frame UV/optical morphologies have comparable specific angularmomentum to disc-dominated galaxies of the same stellar mass, but are clumpierand have higher star-formation rate surface densities. We propose that thepeculiar morphologies in high--redshift systems are driven by higher starformation rate surface densities and higher gas fractions leading to a moreclumpy inter-stellar medium.

From Peculiar Morphologies to Hubble-type Spirals: The relation between galaxy dynamics and morphology in star-forming galaxies at z~1.5