Growth of accreting intermediate mass black hole seeds

Abstract

This communication aims to review the mass assembly history of seed black holes to the present time of accreting intermediate mass black hole (IMBH)-candidates. Given the masses and redshifts at present time of 137 IMBH-candidates collected from the literature, we have undertaken a large series of numerical simulations to achieve this goal. The crux is that, we utilize the microscopic theory of black hole (MTBH), which explores the most important novel aspects expected from considerable change of properties of spacetime continuum at spontaneous breaking of gravitation gauge symmetry far above nuclear density. As a corollary, this theory has smeared out the central singularities of BHs, and makes room for their growth and merging behavior. We compute among the others the masses, the growth-time scales, TBH, and the redshifts of seed BHs. In particular, for the present masses log(M/[M⊙]) = 2.20 to 5.99 of IMBH-candidates, the computed seed masses are ranging from log(Mseed/[M⊙]) = −0.50 to 3.29, with corresponding growth-time scales TBH ranging from log(TBH/[yr]) = 8.82 to 10.09. We derived scaling mass-luminosity relation, by means of which we compute the luminosities of IMBH-candidates ranging from log(L/[erg s−1 ]) = 39.13 to 41.653.