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The treatment of dust attenuation is crucial in order to compare the predictions of galaxy formation models with multiwavelength observations. Most past studies have used either simple analytic prescriptions or full radiative transfer (RT) calculations. Here, we couple star formation histories and morphologies predicted by the semi‐analytic galaxy formation model  morgana  with RT calculations from the spectrophotometric and dust code  grasil  to create a library of galaxy spectral energy distributions from the UV/optical through the far‐infrared, and compare the predictions of the RT calculations with analytic prescriptions. We consider a low‐ and high‐redshift sample, as well as an additional library constructed with empirical, non‐cosmological star formation histories and simple (pure bulge or disc) morphologies. Based on these libraries, we derive fitting formulae for the effective dust optical depth as a function of galaxy physical properties such as metallicity, gas mass and radius. We show that such fitting formulae can predict the  V ‐band optical depth with a scatter smaller than 0.4 dex for both the low‐ and high‐redshift samples, but there is a large galaxy‐to‐galaxy scatter in the shapes of attenuation curves, probably due to geometrical variations, which our simple recipe does not capture well. However, our new recipe provides a better approximation to the  grasil  results at optical wavelength than standard analytic prescriptions from the literature, particularly at high redshift.

Evaluating and improving semi‐analytic modelling of dust in galaxies based on radiative transfer calculations