  Emission from active galactic nuclei (AGNs) is known to play an important
role in the evolution of many galaxies including luminous and ultraluminous
systems (U/LIRGs), as well as merging systems. However, the extent, duration,
and exact effects of its influence are still imperfectly understood. To assess
the impact of AGNs on interacting systems, we present a Spectral Energy
Distribution (SED) analysis of a sample of 189 nearby galaxies. We gather and
systematically re-reduce archival broad-band imaging mosaics from the
ultraviolet to the far-infrared using data from GALEX, SDSS, 2MASS, IRAS, WISE,
Spitzer and Herschel. We use spectroscopy from Spitzer/IRS to obtain fluxes
from fine-structure lines that trace star formation and AGN activity. Utilizing
the SED modelling and fitting tool CIGALE, we derive the physical conditions of
the ISM, both in star-forming regions and in nuclear regions dominated by the
AGN in these galaxies. We investigate how the star formation rates (SFRs) and
the fractional AGN contributions ($f_{\rm{AGN}}$) depend on stellar mass,
galaxy type, and merger stage. We find that luminous galaxies more massive than
about $10^{10} \rm{M}_{*}$ are likely to deviate significantly from the
conventional galaxy main-sequence relation. Interestingly, infrared AGN
luminosity and stellar mass in this set of objects are much tighter than SFR
and stellar mass. We find that buried AGNs may occupy a locus between bright
starbursts and pure AGNs in the $f_{\rm{AGN}}$-[Ne V]/[Ne II] plane. We
identify a modest correlation between $f_{\rm{AGN}}$ and mergers in their later
stages.
