Poster Title: The Growth of SMBHs in Optically-Thick Starburst Galaxies
Abstract: The formation and growth of supermassive balck holes (SMBHs)linked with bulges are considered. We focus on the radiation hydrodynamic process for the growth of SMBH in the optically thick starburst phase (e.g.,ULIRG), where radiation from bulge stars drives the mass accretion on to a galactic center from a galactic scale through radiation drag (Poynting-Robertson)effect. In this scenario, we found that SMBH-to-bulge mass ratio is basically determined by the nuclear energy conversion efficiency from hydrogen to helium, \epsilon=0.007.Furthermore, we have constructed the coevolution model of AGN (accreting BH) and host galaxy. First, we have made this model apply to QSO hosts (ellipticals). As a result, it is found that the AGN luminosity-dominant phase (QSO phase) is preceded by the host luminosity-dominant phase, which is called "proto-QSO phase". This phase corresponds to the early phase with broad emission line width of less than 1500km/s, and can be regarded as a "Narrow line Type I QSO (NLQSO1)". Also, its hosts have massive dusty disks within youger bulges. In addition, it is anticipated by an optically-thick starburst phase (ULIRG). In this phase, the BH mass fraction is predicted to be even less than 0.002.Second, such radiation drag model has been also applied to disk galaxies. As a consequence, we found that the SMBH should be smaller in a disk galaxy, but correlate with the bulge components. Thus, by analogy to proto-QSOs, NLS1s (BH growing phase) may have massive dusty disks within younger bulges. Therefore, the preset model could be a physical picture of evolution of LIRGs(ULIRGs) to Sys (QSOs);LIRGs(ULIRGs)-> NLS1s(NLQSOs)->Sy1s(QSO1s)->LLAGN. Finally, we discuss a possible candidate for NLQSOs by considering theoretical predictions for the observable properties.
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