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Nebular emission lines are critical to measure physical properties in theionized gas (e.g., metallicity, the SFR, or dust attenuation). They alsoaccount for a significant fraction of broadband fluxes, in particular at thehighest redshifts, and therefore can strongly affect the determination of otherphysical properties, such as the stellar mass, which are crucial in shaping ourunderstanding of galaxy formation and evolution. We investigate a sample of 51LBGs at 3.0<z<3.8 with detected [OIII] line emissions and estimated thephysical properties of these galaxies to examine the impact of includingnebular emission data in the SED fitting. We used CIGALE to fit the rest-frameUV-to-NIR SEDs of these galaxies and their emission line data simultaneously.We ran CIGALE with and without the nebular model or the emission line data, andcompare the results to show the importance of including the nebular emissionline data in the SED fitting. We find that without the nebular model, thefitting overestimates the stellar mass due to the strong [OIII] lines that areredshifted to the Ks-band, consistent with previous results. The emission linedata are necessary to constrain the nebular model in the SED fitting. Examiningthe Ks-band excess, which is mostly used to estimate the emissions of the[OIII]+Hb lines when there is no spectral data, we find that the estimation andobservation are statistically consistent. However, the difference can reach upto more than 1 dex in some catastrophic cases, which shows the importance ofobtaining spectroscopic measurements for these lines. We also estimate theequivalent width of the Hb absorption and find it negligible compared to the Hbemission. We conclude that line emission is important to constrain the nebularmodels and to obtain reliable estimates of the physical properties of galaxies.These data should be taken into account in the SED fitting.

Properties of LBGs with [OIII] detection at z $\sim$ 3.5: The importance of including nebular emission data in SED fitting