As part of our Spitzer Spirals , Bridges , and Tails project to help understand the effects of galaxy interactions on star formation , we analyze GALEX ultraviolet , SARA optical , and Spitzer infrared images of the interacting galaxy pair Arp 82 ( NGC 2535/6 ) and compare to a numerical simulation of the interaction .
We investigate the multi-wavelength properties of several individual star forming complexes ( clumps ) .
Using optical and UV colors , EW ( H \alpha ) , and population synthesis models we constrain the ages of the clumps and find that the median clump age is \sim 9 Myr .
The clumps have masses ranging from a few \times 10 ^ { 6 } to 10 ^ { 9 } M _ { \odot } .
In general , the clumps in the tidal features have similar ages to those in the spiral region , but are less massive .
The clumps provide 33 % , 36 % , and 70 % of the FUV , 8.0 \mu m , and 24 \mu m emission , respectively .
The 8 \mu m and 24 \mu m luminosities are used to estimate the far-infrared luminosities and the star formation rates of the clumps .
The total clump star formation rate is \sim 2.0 \pm 0.8 M _ { \odot } yr ^ { -1 } , while the entire Arp 82 system is forming stars at a rate of \sim 4.9 \pm 2.0 M _ { \odot } yr ^ { -1 } .
We find , for the first time , stars in the H I arc to the southeast of the NGC 2535 disk .
Population synthesis models indicate that all of the observed populations have young to intermediate ages .
We conclude that although the gas disks and some old stars may have formed early-on , the progenitors may have been late-type or low surface brightness and the evolution of these galaxies seems to have halted until the recent encounter .