Morphological and photometric evolution of ultraluminous infrared galaxies: The nature of faint scuba sources

We investigate when and how a dusty starburst galaxy merger can be heavily obscured by dust and consequently becomes an ultraluminous infrared galaxy (ULIRG), based on numerical simulations of chemodynamical and photometric evolution of dusty gas-rich major galaxy mergers. We found that a major galaxy merger is more likely to become a ULIRG preferentially in the merger late phase, when the two disks become very close and the very high density dusty gas can obscure heavily the central secondary massive starburst. We furthermore show how the optical and near-infrared morphology of a simulated ULIRG at intermediate (z = 0.4) and high redshift (z = 1-2) can be observed by the Hubble Space Telescope (HST) in order to present a plausible explanation for the origin of some host galaxies of the faint SCUBA sources recently observed by Small et al. The results of our numerical simulations imply that some SCUBA sources with apparently faint and compact HST morphology can be higher redshift dust-enshrouded starburst mergers with their outer low surface brightness tidal features hardly detectable in the present optics of the HST.