rates on redshift can largely be ignored. The approximation will become increasingly inaccurate for high-mass binaries, such as those comprising one or two BHs. In Sections \[sec:IMR\] and \[sec:fullrates\] we went beyond this approximation by implementing three “complete” IMR waveform models (EOB, PhC, PhB), and we described how to combine these models with simulations from the [StarTrack]{} code in order to obtain more accurate estimates of the event rates (see Eq. (\[eq:rate\])).

The analytical estimates of Section \[sec:simplerates\] with local merger rates based on the [StarTrack]{} code are presented in Table \[tab:simplerates\]. The more careful event rate calculations of Section \[sec:fullrates\] are listed in Table \[rates2genH\] (for the high-end metallicity scenario) and Table \[rates2genL\] (for the low-end metallicity scenario).

In these tables, the “single-detector” columns represent estimated detection rates for a single detector with a $\rho \ge 8$ threshold for detectability. This is often used as a proxy for rates in multi-detector networks [@2010CQGra..27q3001A]. In the “three-detector” columns we consider two alternate detectability thresholds: minimum [*network*]{} SNRs of either 10 or 12 for a three-detector network composed of three instruments located at the LIGO Hanford, LIGO Livingston, and Virgo sites, all with aLIGO sensitivity. The network SNR threshold of 10 