We present 0 \farcs 2 resolution near-infrared integral field spectroscopy of H \alpha  emission from six star forming galaxies at z \sim 1.6 ( look-back time of \sim 9.6 Gyr ) .
These observations were obtained with OSIRIS using the Keck Laser Guide Star Adaptive Optics system .
All sources have a compact spatial extent of \sim 1 \arcsec , with an average half light radius of \overline { r } _ { 1 / 2 } =2.9 kpc and average dereddened star formation rate of 22 M _ { \odot } Â yr ^ { -1 } .
Based on H \alpha  kinematics we find that these six galaxies are dynamically distinguishable , and we classify them as either merger or disk candidate systems .
We find three merger systems ( HDF-BX1287 , HDF-BX1315 , and Q1623-BX491 ) with varying geometries and dynamical properties .
Three galaxies ( HDF-BMZ1299 , Q2343-BX344 , and Q2343-BM145 ) are well-fit by an inclined-disk model with low velocity residuals ( 20 to 46 km s ^ { -1 } ) .
An average plateau velocity of \overline { v _ { p } } =185 km s ^ { -1 } Â is achieved within 1.0 kpc .
The majority of observed velocity dispersions ( \overline { \sigma } \sim 88 km s ^ { -1 } ) can be explained by the residual seeing halo , and are not intrinsic to our sources .
However , one merger and one disk candidate have high velocity dispersions ( \sigma _ { obs } \gtrsim 200 km s ^ { -1 } ) that can not be solely explained by beam smearing .
For two disk candidates , we detect [ N ii ]  emission and are able to map the [ N ii ] /H \alpha  ratio on kiloparsec scales .
In both cases , [ N ii ]  emission is more concentrated than H \alpha  emission ( \lesssim 0 \farcs 2 ) , and peak ratios are best explained by the presence of an AGN .
These are among the weakest known AGN at high redshift , however their emission is strong enough to impact high redshift metallicity studies that use nebular ratios .
All disk candidates have likely completed only a few orbital periods , and if left unperturbed are excellent candidates to become present-day spiral galaxies .