  We perform SED fitting analysis on a COSMOS sample covering UV-to-FIR
wavelengths with emission lines from the FMOS survey. The sample of 182 objects
with H$\alpha$ and [OIII]$\lambda5007$ emission spans over a range of
$1.40<\rm{z}<1.68$. We obtain robust estimates of stellar mass
($10^{9.5}-10^{11.5}~\rm{M_\odot}$) and SFR
($10^1-10^3~\rm{M_\odot}~\rm{yr}^{-1}$) from the Bayesian analysis with CIGALE
fitting continuum photometry and H$\alpha$. We obtain a median attenuation of
A$_\rm{H\alpha}=1.16\pm0.19$ mag and A$_\rm{[OIII]}=1.41\pm0.22$ mag. H$\alpha$
and [OIII]$\lambda5007$ attenuations are found to increase with stellar mass,
confirming previous findings. A difference of $57$% in the attenuation
experienced by emission lines and continuum is found in agreement with the
lines being more attenuated than the continuum. New CLOUDY HII-region models in
CIGALE enable good fits of H$\alpha$, H$\beta$, [OIII]$\lambda5007$ emission
lines with differences smaller than $0.2$ dex. Fitting [NII]$\lambda6584$ line
is challenging due to well-known discrepancies in the locus of galaxies in the
BPT diagram at intermediate redshifts. We find a positive correlation for SFR
and dust-corrected L$_\rm{[OIII]\lambda5007}$ and we derive the linear relation
$\log_{10}\rm{(SFR/\rm{M}_\odot~\rm{yr}^{-1})}=\log_{10}
(\rm{L}_{[\rm{OIII]}}/\rm{ergs~s^{-1}})-(41.20\pm0.02)$. Leaving the slope as a
free parameter leads to
$\log_{10}\rm{(SFR/\rm{M}_\odot~\rm{yr}^{-1})}=(0.83\pm0.06)\log_{10}(\rm{L}_{[\rm{OIII]}}/\rm{ergs~s^{-1}})-(34.01\pm2.63)$.
Gas-phase metallicity and ionization parameter variations account for a $0.24$
dex and $1.1$ dex of the dispersion, respectively. An average value of
$\log\rm{U}\approx-2.85$ is measured for this sample. Including HII-region
models to fit simultaneously photometry and emission line fluxes are paramount
to analyze future data from surveys such as MOONS and PFS.
