Fitting spectral energy distributions of FMOS-COSMOS emission-line galaxies at<i>z</i>∼ 1.6: Star formation rates, dust attenuation, and [OIII]<i>λ</i>5007 emission-line luminosities

We perform a spectral energy distribution fitting analysis on COSMOS photometric sample covering the ultra-violet up to far-infrared wavelengths and including emission lines from Fiber Multi-Object Spectrograph survey. The consists of 182 objects with H α [OIII] λ 5007 line measurements lying in redshift range 1.40 &lt; z 1.68. obtain robust estimates stellar mass star-formation rate spanning over 10 9.5 − 11.5 M ⊙ 1 3 yr −1 Bayesian performed CIGALE using continuum photometry fluxes. Combining spectroscopy gives secure estimations amount dust attenuation for both emissions. median A = 1.16 ± 0.19 mag 1.41 0.22 mag. attenuations are found increase mass, confirming previous findings . difference 57% experienced by is be agreement being more attenuated than emission. Implementation new CLOUDY HII-region models enables good fits , β discrepancies smaller 0.2 dex predicted Fitting [NII] 6584 challenging due well-known locus galaxies [NII]-BPT diagram at intermediate high redshifts. find positive correlation between SFR L after correcting we derive linear relation log (SFR/ )=log ( [OIII]/ergs s )−(41.20 0.02). Leaving slope as free parameter leads )=(0.83 0.06)log (L /ergs )−(34.01 2.63). spread driven differences gas-phase metallicity ionization accounting 0.24 1.1 dispersion, respectively. report an average value U ≈ −2.85 this galaxies. Including fit simultaneously data fluxes paramount analyses upcoming sets large spectroscopic surveys future, such MOONS PFS.