Top panels: Best-fit models of the ULIRGs in our sample (observed-frame). The IRAS name of the galaxy is indicated in the top left-hand corner. The blue line shows the unattenuated stellar spectrum, and the black line shows the total SED including the attenuated stellar spectrum and the emission from dust in the infrared. The red squares are the available observed broad-band luminosities, and the green line is the observed Spitzer/IRS spectrum of this galaxy. The residuals are shown at the bottom of the panel. Bottom panels: Likelihood distributions of physical quantities derived from our fit to the observed SED: fraction of the total IR luminosity contributed by dust in the diffuse ISM (f_μ); total effective V-band absorption optical depth of dust (); fraction of the total V-band absorption optical depth of the dust contributed by the diffuse ISM (μ); effective V-band absorption optical depth of dust in the ambient ISM (); specific star formation rate (ψ_S); stellar mass (M_∗) and dust mass (M_d); total dust IR luminosity (); global contributions by PAHs (), the hot mid-IR continuum () and warm dust to (); temperature of warm dust in stellar birth clouds (); contribution by cold dust to (), and temperature of cold dust in the diffuse ISM ().