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Using the combined resolving power of the Hubble Space Telescope andgravitational lensing, we resolve star-forming structures in a z~2.5 galaxy onscales much smaller than the usual kiloparsec diffraction limit of HST. SGASJ111020.0+645950.8 is a clumpy, star forming galaxy lensed by the galaxycluster SDSS J1110+6459 at z = 0.659, with a total magnification ~30x acrossthe entire arc. We use a hybrid parametric/non-parametric strong lensing massmodel to compute the deflection and magnification of this giant arc,reconstruct the light distribution of the lensed galaxy in the source plane,and resolve the star formation into two dozen clumps. We develop aforward-modeling technique to model each clump in the source plane. We raytrace the model to the image plane, convolve with the instrumental point spreadfunction (PSF), and compare with the GALFIT model of the clumps in the imageplane, which decomposes clump structure from more extended emission. Thistechnique has the advantage, over ray tracing, by accounting for the asymmetriclensing shear of the galaxy in the image plane and the instrument PSF. At thisresolution, we can begin to study star formation on a clump-by-clump basis,toward the goal of understanding feedback mechanisms and the buildup ofexponential disks at high redshift.

Star Formation at z=2.481 in the Lensed Galaxy SDSS J1110+6459, I: Lens Modeling and Source Reconstruction