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For lensed galaxy SGAS J111020.0+645950.8 at redshift z=2.481, which ismagnified by a factor of 28 +- 8, we analyze the morphology of star formationas traced by rest-frame ultraviolet emission, in both the highly-magnifiedsource plane, and in simulations of how this galaxy would appear withoutlensing magnification. Were this galaxy not lensed but drawn from an HST deepfield, we would conclude that almost all its star formation arises from anexponential disk (S\'ersic index of 1.0 +- 0.4) with an effective radius of r_e= 2.7 +- 0.3 kpc measured from two-dimensional fitting to F606W using Galfit,and r_e=1.9 +- 0.1 kpc measured by fitting a radial profile to F606W ellipticalisophotes. At the normal spatial resolution of the deep fields, there is nosign of clumpy star formation within SGAS J111020.0+645950.8 . However, theenhanced spatial resolution enabled by gravitational lensing tells a verydifferent story: much of the star formation arises in two dozen clumps withsizes of r=30--50 pc spread across the 7 kpc length of the galaxy. The colorand spatial distribution of the diffuse component suggests that still smallerclumps are unresolved. Despite this clumpy, messy morphology, the radialprofile is still well-characterized by an exponential profile. In this lensedgalaxy, stars are forming in complexes with sizes well below 100 pc; such sizesare wholly unexplored by surveys of galaxy evolution at 1<z<3.

Star Formation at z=2.481 in the Lensed Galaxy SDSS J1110+6459, II: What is missed at the normal resolution of the Hubble Space Telescope?