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In this paper, we combine the stellar spectral synthesis code STARBURST 99,the nebular modelling code MAPPINGS IIIq, a 1-D dynamical evolution model of\HII regions around massive clusters of young stars and a simplified model ofsynchrotron emissivity to produce purely theoretical self-consistent syntheticspectral energy distributions (SEDs) for (solar metallicity) starbursts lastingsome $10^8$ years. These SEDs extend from the Lyman Limit to beyond 21 cm. Wefind that two ISM parameters control the form of the SED; the pressure in thediffuse phase of the ISM (or, equivalently, its density), and the molecularcloud dissipation timescale. We present detailed SED fits to Arp 220 and NGC6240, and we give the predicted colors for starburst galaxies derived from ourmodels for the IRAS and the Spitzer Space Observatory MIPS and IRACinstruments. Our models reproduce the spread in observed colors of starburstgalaxies. Finally, we present absolute calibrations to convert observed fluxesinto star formation rates in the UV (GALEX), at optical wavelengths(H$\alpha$), and in the IR (IRAS or the Spitzer Space Observatory). (AbstractTruncated)

Modeling the Pan–Spectral Energy Distribution of Starburst Galaxies. I. The Role of ISM Pressure and the Molecular Cloud Dissipation Timescale