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On the Prevalence of Supermassive Black Holes over Cosmic Time

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Academic year: 2020

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Figure

Figure 1. Number of 10 10 M e halos that built a z =0 halo. At each halo mass bin, we count the number of progenitors that merged into each halo
Figure 3 shows the occupation fraction predictions for M c =10 10 M e . The comparison with the observational lower limit implies p 30%, with lower seed probabilities ruled out.
Figure 3. Black hole occupation in the local universe as a function of stellar mass. Differently colored model curves correspond to different seeding probabilities p.
Figure 5. Left panel: the birth rate of black holes over cosmic time. Curves show different seeding fractions p and mass thresholds M 0
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