http://arxiv.org/abs/1604.05317
We show influences of the mass of seed black holes on black hole mass — bulge mass relation at z ~ 0 by using a semi-analytic model of galaxy formation combined with large cosmological N-body simulations. We constrain our model to reproduce observed properties of galaxies at z ~ 0. Similar to other semi-analytic models, we place a seed black hole immediately after a galaxy forms. When we set the seed black hole mass to 10^5 M_sun, we find that the model result becomes inconsistent with recent observational results of black hole mass — bulge mass relation for dwarf galaxies. Namely, the model predicts that bulges with ~ 10^9 M_sun harbor black holes more massive than observed. On the other hand, when we employ seed black holes with 10^3 M_sun or randomly choose their masses in the range of 10^{3-5} M_sun, the black hole mass — bulge mass relation obtained from these models are consistent with observational results including dispersions. We find that to obtain more stringent restrictions of the mass of seed black holes, observations of less massive bulges at z ~ 0 are more powerful than that of black hole mass — bulge mass relations at higher redshifts.
H. Shirakata, T. Kawaguchi, T. Okamoto, et. al.
Wed, 20 Apr 16
10/71
Comments: 6 pages, 2 tables, 4 figures. Submitted to MNRAS Letter. Comments are welcome
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