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We have identified 1027 star forming complexes in a sample of 46 galaxiesfrom the Spirals, Bridges, and Tails (SB&T) sample of interacting galaxies, and693 star forming complexes in a sample of 38 non-interacting spiral (NIS)galaxies in $8\rm{\mu m}$ observations from the Spitzer Infrared Array Camera.We have used archival multi-wavelength UV-to IR observations to fit theobserved spectral energy distribution (SED) of our clumps with the CodeInvestigating GALaxy Emission (CIGALE) using a double exponentially declinedstar formation history (SFH). We derive SFRs, stellar masses, ages andfractions of the most recent burst, dust attenuation, and fractional emissiondue to an AGN for these clumps. The resolved star formation main sequence holdson 2.5kpc scales, although it does not hold on 1kpc scales. We analyzed therelation between SFR, stellar mass, and age of the recent burst in the SB&T andNIS samples, and we found that the SFR per stellar mass is higher in the SB&Tgalaxies, and the clumps are younger in the galaxy pairs. We analyzed the SFRradial profile and found that SFR is enhanced through the disk and in the tidalfeatures relative to normal spirals.

Stellar Population Synthesis of star forming clumps in galaxy pairs and non-interacting spiral galaxies