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The goal of population spectral synthesis (PSS) is to decipher from thespectrum of a galaxy the mass, age and metallicity of its constituent stellarpopulations. This technique has been established as a fundamental tool inextragalactic research. It has been extensively applied to large spectroscopicdata sets, notably the SDSS, leading to important insights into the galaxyassembly history. However, despite significant improvements over the pastdecade, all current PSS codes suffer from two major deficiencies that inhibitus from gaining sharp insights into the star-formation history (SFH) ofgalaxies and potentially introduce substantial biases in studies of theirphysical properties (e.g., stellar mass, mass-weighted stellar age and specificstar formation rate). These are i) the neglect of nebular emission in spectralfits, consequently, ii) the lack of a mechanism that ensures consistencybetween the best-fitting SFH and the observed nebular emission characteristicsof a star-forming (SF) galaxy. In this article, we present FADO (FittingAnalysis using Differential evolution Optimization): a conceptually novel,publicly available PSS tool with the distinctive capability of permittingidentification of the SFH that reproduces the observed nebular characteristicsof a SF galaxy. This so-far unique self-consistency concept allows us tosignificantly alleviate degeneracies in current spectral synthesis. Theinnovative character of FADO is further augmented by its mathematicalfoundation: FADO is the first PSS code employing genetic differential evolutionoptimization. This, in conjunction with other unique elements in itsmathematical concept (e.g., optimization of the spectral library usingartificial intelligence, convergence test, quasi-parallelization) results inkey improvements with respect to computational efficiency and uniqueness of thebest-fitting SFHs.

astronomy and astrophysics

Fitting Analysis using Differential Evolution Optimization (FADO):  Spectral population synthesis through genetic optimization under  self-consistency boundary conditions