The AGN contribution to the UV-FIR luminosities of interacting galaxies
  and its role in identifying the Main Sequence
  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.
