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Spectral synthesis is a powerful tool for interpreting the physicalproperties of galaxies by decomposing their spectral energy distributions intothe main luminosity contributors (e.g. stellar populations or ionised gas).However, the impact nebular emission has on the inferred properties ofstar-forming (SF) galaxies has been largely overlooked over the years. Theobjective of this work is to estimate the relations between stellar propertiesof SF galaxies from SDSS DR7 by simultaneously fitting the stellar and nebularcontinua with FADO and comparing them to the results derived using STARLIGHT, arepresentative of purely stellar population synthesis codes. Differencesbetween codes regarding average mass, mean age and mean metallicity values cango as high as $\sim$0.06 dex for the overall population of galaxies and$\sim$0.12 dex for SF galaxies (galaxies with EW(H$\alpha$)>3 \AA), with themost prominent difference between both codes in the light-weighted mean stellarage. A closer look into the average light- and mass-weighted star formationhistories of intensively SF galaxies (EW(H$\alpha$)>75 \AA) suggests thatSTARLIGHT is underestimating the average light-weighted age of intensively SFgalaxies by up to $\sim$0.17 dex and overestimating the light-weightedmetallicity by up to $\sim$0.13 dex compared to FADO (or vice versa). Thecomparison between the average stellar properties of passive, SF andintensively SF galaxy samples also reveals that differences between codesincrease with increasing EW(H$\alpha$) and decreasing total stellar mass. Thiswork finds indirect evidence that a purely stellar population synthesisapproach negatively impacts the inferred stellar properties of galaxies withrelatively high star formation rates. In turn, this can bias interpretations offundamental relations such as the mass-age or mass-metallicity.

Revisiting stellar properties of star-forming galaxies with stellar and nebular spectral modelling