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We present an application of the da Cunha, Charlot & Elbaz (2008) model ofthe spectral energy distribution (SEDs) of galaxies from the ultraviolet tofar-infrared to a small pilot sample of purely star-forming Ultra-LuminousInfrared Galaxies (ULIRGs). We interpret the observed SEDs of 16 ULIRGs usingthis physically-motivated model which accounts for the emission of stellarpopulations from the ultraviolet to the near-infrared and for the attenuationby dust in two components: an optically-thick starburst component and thediffuse ISM. The infrared emission is computed by assuming that all the energyabsorbed by dust in these components is re-radiated at mid- and far-infraredwavelengths. This model allows us to derive statistically physical propertiesincluding star formation rates, stellar masses, as well as temperatures andmasses of different dust components and plausible star formation histories. Wefind that, although the ultraviolet to near-infrared emission represents only asmall fraction of the total power radiated by ULIRGs, observations in thiswavelength range are important to understand the properties of the stellarpopulations and dust attenuation in the diffuse ISM of these galaxies.Furthermore, our analysis indicates that the use of mid-infrared spectroscopyfrom the Infrared Spectrograph on the Spitzer Space Telescope is crucial toobtain realistic estimates of the extinction to the central energy source,mainly via the depth of the 9.7-micron silicate feature, and thus accuratelyconstrain the total energy balance. Our findings are consistent with the notionthat, in the local Universe, the physical properties of ULIRGs arefundamentally different from those of galaxies with lower infrared luminositiesand that local ULIRGs are the result of merger-induced starbursts. [abridged]

Exploring the physical properties of local star-forming ULIRGs from the ultraviolet to the infrared