Stellar Population Synthesis of star forming clumps in galaxy pairs and
  non-interacting spiral galaxies
  We have identified 1027 star forming complexes in a sample of 46 galaxies
from the Spirals, Bridges, and Tails (SB&T) sample of interacting galaxies, and
693 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 the
observed spectral energy distribution (SED) of our clumps with the Code
Investigating GALaxy Emission (CIGALE) using a double exponentially declined
star formation history (SFH). We derive SFRs, stellar masses, ages and
fractions of the most recent burst, dust attenuation, and fractional emission
due to an AGN for these clumps. The resolved star formation main sequence holds
on 2.5kpc scales, although it does not hold on 1kpc scales. We analyzed the
relation between SFR, stellar mass, and age of the recent burst in the SB&T and
NIS samples, and we found that the SFR per stellar mass is higher in the SB&T
galaxies, and the clumps are younger in the galaxy pairs. We analyzed the SFR
radial profile and found that SFR is enhanced through the disk and in the tidal
features relative to normal spirals.
