{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,2,14]],"date-time":"2026-02-14T01:53:58Z","timestamp":1771034038023,"version":"3.50.1"},"reference-count":122,"publisher":"EDP Sciences","license":[{"start":{"date-parts":[[2019,1,28]],"date-time":"2019-01-28T00:00:00Z","timestamp":1548633600000},"content-version":"vor","delay-in-days":0,"URL":"https:\/\/www.edpsciences.org\/en\/authors\/copyright-and-licensing"}],"content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["A&amp;A"],"accepted":{"date-parts":[[2018,11,13]]},"published-print":{"date-parts":[[2019,2]]},"abstract":"<jats:p><jats:italic>Context.<\/jats:italic>Spectral population synthesis (<jats:monospace>PS<\/jats:monospace>) is a fundamental tool in extragalactic research that aims to decipher the assembly history of galaxies from their spectral energy distribution (SED). Whereas this technique has led to key insights into galaxy evolution in recent decades, star formation histories (SFHs) inferred therefrom have been plagued by considerable uncertainties stemming from inherent degeneracies and the fact that until recently all<jats:monospace>PS<\/jats:monospace>codes were restricted to purely stellar fits, neglecting the essential contribution of nebular emission (ne). With the advent of<jats:sc>FADO<\/jats:sc>(Fitting Analysis using Differential evolution Optimisation), the now possible self-consistent modelling of stellar and<jats:monospace>ne<\/jats:monospace>opens new routes to the exploration of galaxy SFHs.<\/jats:p><jats:p><jats:italic>Aims.<\/jats:italic>The main goal of this study is to quantitatively explore the accuracy to which<jats:sc>FADO<\/jats:sc>can recover physical and evolutionary properties of galaxies and compare its output with that from purely stellar<jats:monospace>PS<\/jats:monospace>codes.<\/jats:p><jats:p><jats:italic>Methods.<\/jats:italic><jats:sc>FADO<\/jats:sc>and<jats:sc>STARLIGHT<\/jats:sc>were applied to synthetic SEDs that track the spectral evolution of stars and gas in extinction-free mock galaxies of solar metallicity that form their stellar mass (<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub>) according to different parametric SFHs. Spectral fits were computed for two different set-ups that approximate the spectral range of SDSS and CALIFA (V500) data, using up to seven libraries of simple stellar population spectra in the 0.005\u20132.5<jats:italic>Z<\/jats:italic><jats:sub>\u2299<\/jats:sub>metallicity range.<\/jats:p><jats:p><jats:italic>Results.<\/jats:italic>Our analysis indicates that<jats:sc>FADO<\/jats:sc>can recover the key physical and evolutionary properties of galaxies, such as<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub>and mass- and light-weighted mean age and metallicity, with an accuracy better than 0.2 dex. This is the case even in phases of strongly elevated specific star formation rate (sSFR) and thus with considerable<jats:monospace>ne<\/jats:monospace>contamination (EW(H<jats:italic>\u03b1<\/jats:italic>)\u2004&gt; \u200410<jats:sup>3<\/jats:sup>\u00c5). Likewise, population vectors from<jats:sc>FADO<\/jats:sc>adequately recover the mass fraction of stars younger than 10 Myr and older than 1 Gyr (<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub><jats:sup>&lt;10<jats:italic>Myr<\/jats:italic><\/jats:sup>\/<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub><jats:sup>total<\/jats:sup>and<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub><jats:sup>&gt;1<jats:italic>Gyr<\/jats:italic><\/jats:sup>\/<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub><jats:sup>total<\/jats:sup>, respectively) and reproduce with a high fidelity the observed H<jats:italic>\u03b1<\/jats:italic>luminosity. As for<jats:sc>STARLIGHT<\/jats:sc>, our analysis documents a moderately good agreement with theoretical values only for evolutionary phases for which<jats:monospace>ne<\/jats:monospace>drops to low levels (EW(H<jats:italic>\u03b1<\/jats:italic>)\u2004\u2264\u200460 \u00c5) which, depending on the assumed SFH, correspond to an age between \u223c0.1 Gyr and 2\u20134 Gyr. However, fits with<jats:sc>STARLIGHT<\/jats:sc>during phases of high sSFR severely overestimate both<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub>and the mass-weighted stellar age, whereas strongly underestimate the light-weighted age and metallicity. Furthermore, our analysis suggests a subtle tendency of<jats:sc>STARLIGHT<\/jats:sc>to favour a bi-modal SFH, as well a slightly overestimated<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub><jats:sup>&lt;10<jats:italic>Myr<\/jats:italic><\/jats:sup>\/<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub><jats:sup>total<\/jats:sup>, regardless of galaxy age. Whereas the amplitude of these biases can be reduced, depending on the specifics of the fitting procedure (e.g. accuracy and completeness of flagging emission lines, omission of the Balmer and Paschen jump from the fit), they persist even in the idealised case of a line-free SED comprising only stellar and nebular continuum emission.<\/jats:p><jats:p><jats:italic>Conclusions.<\/jats:italic>The insights from this study suggest that the neglect of nebular continuum emission in<jats:sc>STARLIGHT<\/jats:sc>and similar purely stellar<jats:monospace>PS<\/jats:monospace>codes could systematically impact<jats:italic>M<\/jats:italic><jats:sub>\u22c6<\/jats:sub>and SFH estimates for star-forming galaxies. We argue that these biases can be relevant in the study of a range of topics in extragalactic research, including the redshift-dependent slope of the star formation (SF) main sequence, the SF frosting hypothesis, and the regulatory role of supermassive black holes on the global SFH of galaxies.<\/jats:p>","DOI":"10.1051\/0004-6361\/201833438","type":"journal-article","created":{"date-parts":[[2018,12,18]],"date-time":"2018-12-18T10:00:02Z","timestamp":1545127202000},"page":"A56","source":"Crossref","is-referenced-by-count":20,"title":["Self-consistent population spectral synthesis with FADO"],"prefix":"10.1051","volume":"622","author":[{"given":"Leandro S. 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