waveform models and different detector sensitivities, representative of aLIGO, AdV, and KAGRA. Several different groups have presented similar estimates and studies in the past decade [e.g., @lipunov1997; @bethe; @dedonder; @bloom; @grishchuk:2001; @nele2001; @voss; @dewi; @nutzman; @pfahl; @danny; @PostnovYungelson:2006; @seba; @mennekens]. However, none have combined cosmological DCO populations with accurate GW models to obtain thorough, detector-specific results. Our astrophysical models for DCO formation are reviewed in Section \[binevol\]. Gravitational waveform models and signal-to-noise ratio estimates are discussed in Section \[wmodels\]. Our procedure to compute event rates is presented in Section \[sec:fullrates\]. Event rates and bulk properties of the detected populations are presented in Section \[sec:results\]. In Section \[sec:nobhbh\] we present and discuss the study by [@mennekens], the primary result of which is the lack of detectable BH-BH systems. In Section \[sec:conclusions\] we discuss the possible astrophysical payoff of the first GW detections and important directions for future work.

Astrophysical models {#binevol}
====================

Binary evolution
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We begin with a summary of the four [StarTrack]{} evolutionary models that form the backbone of this work; a more detailed discussion can be found in [@dominik; @dominik2].

*1) Standard model*. This is our reference model, representing the state of the art in the formation and 