We present results from IROCKS ( Intermediate Redshift OSIRIS Chemo-Kinematic Survey ) for sixteen z \sim 1 and one z \sim 1.4 star-forming galaxies .
All galaxies were observed with OSIRIS with the laser guide star adaptive optics system at Keck Observatory .
We use rest-frame nebular H \alpha emission lines to trace morphologies and kinematics of ionized gas in star-forming galaxies on sub-kiloparsec physical scales .
We observe elevated velocity dispersions ( \sigma \gtrsim 50 km s ^ { -1 } ) seen in z > 1.5 galaxies persist at z \sim 1 in the integrated galaxies .
Using an inclined disk model and the ratio of v / \sigma , we find that 1/3 of the z \sim 1 sample are disk candidates while the other 2/3 of the sample are dominated by merger-like and irregular sources .
We find that including extra attenuation towards HII regions derived from stellar population synthesis modeling brings star formation rates ( SFR ) using H \alpha and stellar population fit into a better agreement .
We explore properties of compact H \alpha sub-component , or ” clump , ” at z \sim 1 and find that they follow a similar size-luminosity relation as local HII regions but are scaled-up by an order of magnitude with higher luminosities and sizes .
Comparing the z \sim 1 clumps to other high-redshift clump studies , we determine that the clump SFR surface density evolves as a function of redshift .
This may imply clump formation is directly related to the gas fraction in these systems and support disk fragmentation as their formation mechanism since gas fraction scales with redshift .