Spectra of the composite stellar populations for the Bruzual & Charlot (2003; blue) and Maraston (2005; orange models). Both models have an identical SFH generated with the sfh2exp module (t₀ = 13 000 Myr, τ₀ = 7000 Myr, t₁ = 250 Myr, τ₁ = 50 Myr, f = 0.01), a Salpeter (1955) IMF, and a metallicity Z = 0.02. Even if the Maraston (2005) models have been developed to handle the contribution of thermally pulsating asymptotic giant branch stars, there are also clear differences at all wavelengths. Such differences are strongly dependent on the actual SFH and the differences seen in this plot are not necessarily representative of what would be obtained with another SFH.