Fig. 8
Left: BHAR/M∗ rate vs. sSFR contours obtained from the simulations presented in Volonteri et al. (2015a). In red the stochastic phase, in yellow the merger phase, and in black the remnant phase. Right: BHAR/M∗ vs. sSFR contours observed in COSMOS in five redshift bins. Sources that are in a major merger state in the first three redshift bins are marked with black stars.
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