Fitting spectral energy distributions of FMOS-COSMOS emission-line galaxies at z$sim$1.6: Star formation rates, dust attenuation, and [OIII]$lambda$5007 emission-line luminosities. (arXiv:2108.13321v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Villa_Velez_J/0/1/0/all/0/1">J. A. Villa-V&#xe9;lez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buat_V/0/1/0/all/0/1">V. Buat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Theule_P/0/1/0/all/0/1">P. Theul&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boquien_M/0/1/0/all/0/1">M. Boquien</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burgarella_D/0/1/0/all/0/1">D. Burgarella</a>

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$_rm{Halpha}=1.16pm0.19$ mag and A$_rm{[OIII]}=1.41pm0.22$ 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
$log_{10}rm{(SFR/rm{M}_odot~rm{yr}^{-1})}=log_{10}
(rm{L}_{[rm{OIII]}}/rm{ergs~s^{-1}})-(41.20pm0.02)$. Leaving the slope as a
free parameter leads to
$log_{10}rm{(SFR/rm{M}_odot~rm{yr}^{-1})}=(0.83pm0.06)log_{10}(rm{L}_{[rm{OIII]}}/rm{ergs~s^{-1}})-(34.01pm2.63)$.
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
$logrm{U}approx-2.85$ 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.

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$_rm{Halpha}=1.16pm0.19$ mag and A$_rm{[OIII]}=1.41pm0.22$ 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
$log_{10}rm{(SFR/rm{M}_odot~rm{yr}^{-1})}=log_{10}
(rm{L}_{[rm{OIII]}}/rm{ergs~s^{-1}})-(41.20pm0.02)$. Leaving the slope as a
free parameter leads to
$log_{10}rm{(SFR/rm{M}_odot~rm{yr}^{-1})}=(0.83pm0.06)log_{10}(rm{L}_{[rm{OIII]}}/rm{ergs~s^{-1}})-(34.01pm2.63)$.
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
$logrm{U}approx-2.85$ 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.

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