We present the rest-frame UV wavelength dependence of the Petrosian-like half-light radius ( r _ { 50 } ) , and the concentration parameter for a sample of 198 star-forming galaxies at 0.5 < z < 1.5 .
We find a \sim 5 % decrease in r _ { 50 } from 1500 Å to 3000 Å , with half-light radii at 3000 Å ranging from 0.6 kpc to 6 kpc .
We also find a decrease in concentration of \sim 0.07 ( 1.9 < C _ { 3000 } < 3.9 ) .
The lack of a strong relationship between r _ { 50 } and wavelength is consistent with a model in which clumpy star formation is distributed over length scales comparable to the galaxy ’ s rest-frame optical light .
While the wavelength dependence of r _ { 50 } is independent of size at all redshifts , concentration decreases more sharply in the far-UV ( \sim 1500 Å ) for large galaxies at z \sim 1 .
This decrease in concentration is caused by a flattening of the inner \sim 20 % of the light profile in disk-like galaxies , indicating that the central regions have different UV colors than the rest of the galaxy .
We interpret this as a bulge component with older stellar populations and/or more dust .
The size-dependent decrease in concentration is less dramatic at z \sim 2 , suggesting that bulges are less dusty , younger , and/or less massive than the rest of the galaxy at higher redshifts .