would have yielded false alarm rates of roughly once per decade in 2009-2010 initial LIGO and Virgo data [see Fig. 3 in @scenarios]. This threshold is optimistic for making confident detections if data quality in advanced detectors is similar to that in the initial detectors and the same searches are used. With this in mind, @scenarios assumed a network SNR threshold of $12$ with an additional threshold constraint on the SNR in the second-loudest instrument; we consider a simple SNR threshold of $12$. Detection rates using a network SNR threshold were calculated using the same framework as above, but implementing a network-geometry-dependent $P(w)$ described (and fitted) in the Appendix. In the order-of-magnitude estimates described by Eq. (\[eq:LocalUniverseMergerRateFormula\]) and provided in Table \[tab:simplerates\] we employ $\left<w^{3}\right> \simeq 0.404$ for the three-detector network ($\rho \ge 10$), a factor of $\sim
4.6$ larger than the value $\left<w^{3}\right> \simeq (1/2.26)^3
\approx 0.0866$ used for a one-detector network.

We now discuss these rate predictions, their dependence on gravitational waveform models, and the astrophysical properties of DCO populations observable by advanced GW detectors.

Broad features of rate estimates
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The main conclusion of this work is that BH-BH mergers should yield the highest detection rates in 