tokens: ≤ 2 redshift range. (b) The same as (a) for 10 examples of each of our three stochastic SFH families. Except for the two very lowest metallicities, increases with redshift in a nearly linear fashion, with little overlap between the tracks for the three SFH families. 5. Summary We combined SSP SEDs from the Starburst99 and BC03 codes for young and old stellar ages, respectively, and generated arrays of CSP SEDs for a large variety of exponentially declining and stochastic SFHs by stacking SSP SEDs as a function of the adopted time-dependent SFRs. For our large suite of models with stochastic SFHs, we take the average metallicity evolution as a function of cosmic age into account. We calculated the intrinsic flux ratios between rest-frame visible–near-IR and rest-frame mid-IR 3.5 μ m on a grid of six metallicities and 16 ages of stellar populations for 13 different SFH families, for 29 visible–near-IR filters, and 5 mid-IR filters with central wavelengths near 3.5 μ m. We find that taking metallicity evolution into account results in significantly higher values at higher redshifts and for higher-metallicity stellar populations at those redshifts. We also provide the range of and for different Hubble types of nearby galaxies, and confirm that our models agree with the observed values. We demonstrated that the method can infer to a level of fidelity that is comparable to that of more established methods. We conclude that the method and its extension, the method presented here, are valid as a first-order dust-correction method, when using the morphology and size of a galaxy as broad a priori constraints to its SFH and redshift, respectively. The method will be applicable to large samples of galaxies for which resolved imagery is available in one rest-frame visible–near-IR filter and one rest-frame λ ∼ 3.5 μ m bandpass. We make our CSP synthesis models and all our results available via a dedicated website in the form of FITS and PNG maps, and ASCII data tables of values as a function of age and metallicity. Appendix A A Set of Distinguishable SSPs We construct our combined model SSP SEDs for a manageably small, yet comprehensive set of parameters that span the range of representative stellar population properties and dust extinction. We consider six metallicity and 16 age values of the stellar population, four extinction laws, and eight V -band extinction values (see Table 6 ). We adopt a grid of 16 stellar population ages between 8 8 In Planck 2015 cosmology (Planck Collaboration et al. 2016 ), the Hubble time t H ≃ 13.8 Gyr. Hence, t = 13.25 Gyr corresponds to 0.55 Gyr after the Big Bang or , consistent with the Planck Collaboration (Paper 2016) results of τ = 0.058 and , so this maximum age is a deliberate choice. 3 Myr and 13.25 Gyr in steps that roughly double for ages between 10 Myr and 10 Gyr. This allows us to follow the rapid evolution of massive stars, without reserving too many SEDs for the slow evolution of low-mass stars. Because the MW
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