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We present an analysis of the 4-2600 $\mu$m spectral energy distributions(SEDs) of the west and east nuclei and the diffuse infrared (IR) region of themerger-driven starburst Arp 220. We examine several possible sourcemorphologies and dust temperature distributions using a mixture of silicate andcarbonaceous grains. From fits to the SEDs we derive dust masses, temperatures,luminosities, and dust inferred gas masses. We show that the west and eastnuclei are powered by central sources deeply enshrouded behind $\sim 10^{26}$cm$^{-2}$ column densities of hydrogen with an exponential densitydistribution, and that the west and east nuclei are optically thick out towavelengths of $\sim 1900$ and $\sim 770$ $\mu$m, respectively. The nature ofthe central sources cannot be determined from our analysis. We derive starformation rates or black hole masses needed to power the IR emission, and showthat the [C II] 158$\mu$m line cannot be used as a tracer of the star formationrate in heavily obscured systems. Dust inferred gas masses are larger thanthose inferred from CO observations, suggesting either larger dust-to-H massratios, or the presence of hidden atomic H that cannot be inferred from COobservations. The luminosities per unit mass in the nuclei are $\sim 450$, insolar units, smaller that the Eddington limit of $\sim 1000 - 3000$ for anoptically thick star forming region, suggesting that the observed gas outflowsare primarily driven by stellar winds and supernova shock waves instead ofradiation pressure on the dust.

Dust masses, compositions, and luminosities in the nuclear disks and the diffuse circumnuclear medium of Arp220