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We present an investigation of clumpy galaxies in the Hubble Ultra Deep Fieldat 0.5 $\leq z \leq$ 1.5 in the rest-frame far-ultraviolet (FUV) using HST WFC3broadband imaging in F225W, F275W, and F336W. An analysis of 1,404 galaxiesyields 209 galaxies that host 403 kpc-scale clumps. These host galaxies appearto be typical star-forming galaxies, with an average of 2 clumps per galaxy andreaching a maximum of 8 clumps. We measure the photometry of the clumps, anddetermine the mass, age, and star formation rates (SFR) utilizing theSED-fitting code FAST. We find that clumps make an average contribution of 19%to the total rest-frame FUV flux of their host galaxy. Individually, clumpscontribute a median of 5% to the host galaxy SFR and an average of $\sim$4% tothe host galaxy mass, with total clump contributions to the host galaxy stellarmass ranging widely from less than 1% up to 93%. Clumps in the outskirts ofgalaxies are typically younger, with higher star formation rates, than clumpsin the inner regions. The results are consistent with clump migration theoriesin which clumps form through violent gravitational instabilities in gas-richturbulent disks, eventually migrate toward the center of the galaxies, andcoalesce into the bulge.

Physical Properties of Sub-galactic Clumps at 0.5 $\leq z \leq$ 1.5 in the UVUDF