http://arxiv.org/abs/1610.09505
Based on a dynamical formation model of a super-massive black-hole (SMBH), we estimate expected observational profile of gravitational wave at ground-based detectors, such as KAGRA or advanced LIGO/VIRGO. Focusing that the second generation of detectors have enough sensitivity from 10 Hz and up (especially with KAGRA due to its location at less seismic noise), we are able to detect the ring-down gravitational wave of a BH of the mass $M < 2 \times 10^3 M_\odot $. This enables us to check the sequence of BH mergers to SMBH via intermediate-mass black-holes (IMBHs). We estimate the number density of galaxies from halo formation model, and estimate the number of BH mergers from giant molecular cloud model assuming hierarchical growth of merged cores. At the designed KAGRA (and/or advanced LIGO/VIRGO), we find that the BH mergers of its total mass $M\sim 60M_\odot$ is at the peak of the expected mass distribution. With its signal-to-noise ratio $\rho=10 (30)$, we estimate the event rate $R \sim 200 (20)$ per year in the most optimistic case, and we also find that BH mergers of the range $M < 150 M_\odot$ are $R>1$ per year for $\rho=10$. Thus if we observe a BH with more than $100 M_\odot$ in future gravitational wave observations, our model naturally explains its source.
H. Shinkai, N. Kanda and T. Ebisuzaki
Tue, 1 Nov 16
63/75
Comments: 9 pages, 10 figures
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