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As part of our Spitzer Spirals, Bridges, and Tails project to help understandthe effects of galaxy interactions on star formation, we analyze GALEXultraviolet, SARA optical, and Spitzer infrared images of the interactinggalaxy pair Arp 82 (NGC 2535/6) and compare to a numerical simulation of theinteraction. We investigate the multiwavelength properties of severalindividual star forming complexes (clumps). Using optical and UV colors,EW(Halpha), and population synthesis models we constrain the ages of the clumpsand find that the median clump age is about 12 Myr. The clumps have massesranging from a few times 10^6 to 10^9 solar masses. In general, the clumps inthe tidal features have similar ages to those in the spiral region, but areless massive. The 8 micron and 24 micron luminosities are used to estimate thefar-infrared luminosities and the star formation rates of the clumps. The totalclump star formation rate is 2.0+/-0.8 solar masses per year, while the entireArp 82 system is forming stars at a rate of 4.9+/-2.0 solar masses per year. Wefind, for the first time, stars in the HI arc to the southeast of the NGC 2535disk. Population synthesis models indicate that all of the observed populationshave young to intermediate ages. We conclude that although the gas disks andsome old stars may have formed early-on, the progenitors are late-type or lowsurface brightness and the evolution of these galaxies was halted until therecent encounter.Comment: Accepted for publication in the AJ, 22 Figures, 5 Table

Large-Scale Star Formation Triggering in the Low-Mass Arp 82 System: A Nearby Example of Galaxy Downsizing Based on UV/Optical/Mid-IR Imaging