Fig. 12
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Eccentricity against semi-major axis for our simulation of the CWD origin binaries. The colour bar shows the number of S-stars predicted for an ejection rate of 10−2 yr−1. In white we show the boundary of the zone of avoidance identified in Burkert et al. (2024). The drop in the number of simulated S-stars at large semi-major axes is due to the selection function from Burkert et al. (2024).
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