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We used the Submillimeter Array (SMA) to image 860 micron continuum andCO(3-2) line emission in the ultraluminous merging galaxy Arp 220, achieving aresolution of 0.23" (80 pc) for the continuum and 0.33" (120 pc) for the line.The CO emission peaks around the two merger nuclei with a velocity signature ofgas rotation around each nucleus, and is also detected in a kpc-size diskencompassing the binary nucleus. The dust continuum, in contrast, is mostlyfrom the two nuclei. The beam-averaged brightness temperature of both line andcontinuum emission exceeds 50 K at and around the nuclei, revealing thepresence of warm molecular gas and dust. The dust emission morphologicallyagrees with the distribution of radio supernova features in the east nucleus,as expected when a starburst heats the nucleus. In the brighter west nucleus,however, the submillimeter dust emission is more compact than the supernovadistribution. The 860 micron core, after deconvolution, has a size of 50-80 pc,consistent with recent 1.3 mm observations, and a peak brightness temperatureof (0.9-1.6)x10^2 K. Its bolometric luminosity is at least 2x10^{11} Lsun andcould be ~10^{12} Lsun depending on source structure and 860 micron opacity,which we estimate to be of the order of tau_{860} ~ 1 (i.e., N_{H_2} ~ 10^{25}cm^{-2}). The starbursting west nuclear disk must have in its center a dustenshrouded AGN or a very young starburst equivalent to hundreds of super starclusters. Further spatial mapping of bolometric luminosity throughsubmillimeter imaging is a promising way to identify the heavily obscuredheating sources in Arp 220 and other luminous infrared galaxies.

SMA Imaging of CO(3-2) Line and 860 micron Continuum of Arp 220 : Tracing the Spatial Distribution of Luminosity