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By means of the updated PARSEC database of evolutionary tracks of massivestars, we compute the integrated stellar light, the ionizing photon budget andthe supernova rates of young simple stellar populations (SSPs), for differentmetallicities and IMF upper mass limits. Using CLOUDY we compute and include inthe SSP spectra the neb- ular emission contribution. We also revisit thethermal and non-thermal radio emission contribution from young stars. UsingGRASIL we can thus predict the panchromatic spectrum and the main recombinationlines of any type of star-forming galaxy, including the effects of dustabsorption and re-emission. We check the new models against the spectral energydistributions (SEDs) of selected well-observed nearby galaxies. From thebest-fit models we obtain a consistent set of star formation rate (SFR)calibrations at wavelengths ranging from ultraviolet (UV) to radio. We alsoprovide analytical calibrations that take into account the dependence onmetallcity and IMF upper mass limit of the SSPs. We show that the latter limitcan be well constrained by combining information from the observed farinfrared, 24 {\mu}m, 33 GHz and H{\alpha} luminosities. Another interestingproperty derived from the fits is that, while in a normal galaxy theattenuation in the lines is significantly higher than that in the nearbycontinuum, in individual star bursting regions they are similar, supporting thenotion that this effect is due to an age selective extinction. Since in theseconditions the Balmer decrement method may not be accurate, we providerelations to estimate the attenuation from the observed 24 {\mu}m or 33 GHzfluxes. These relations can be useful for the analysis of young high redshiftgalaxies.

Modelling the UV to radio SEDs of nearby star-forming galaxies: new Parsec SSP for Grasil