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BINARY BLACK HOLES IN DENSE STAR CLUSTERS: EXPLORING THE THEORETICAL UNCERTAINTIES

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Table 2 Initial Model Parameters
Figure 1 shows the evolution of the core radius (r c ) and the half-mass radius (r h ) for our standard model S
Figure 3. Final SBP at t= 12 Gyr for model S . The dots denote the surface luminosity density
Figure 4. Final number of BHs bound to the cluster, N BH vs. r c,obs ( left ) and r c,obs / r hl,obs ( right ) for all models that survived for at least 11 Gyr
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