to larger distances (making cosmological corrections important) and because, as we discuss below, a large fraction of the SNR for these binaries comes from the merger/ringdown portion of the signal.

Including merger and ringdown {#sec:IMR}
-----------------------------

In order to refine our rate estimates for high-mass systems containing BHs, it is important to consider the full waveform, including inspiral, merger, and ringdown (IMR). The calculation of gravitational waveforms from merging BH-BH and BH-NS binaries requires expensive numerical relativity simulations, but several semi-analytical models have been tuned to reproduce the amplitude and phasing of BH-BH and BH-NS merger simulations. To estimate systematic uncertainties and the impact of spin, we performed rate calculations using three models: (1) the IMRPhenomB model described in [@PhenomB], one of the earliest phenomenological models tuned to both nonspinning and spinning BH-BH simulations with aligned spins, henceforth abbreviated as PhB; (2) the IMRPhenomC (henceforth abbreviated PhC) model by [@santamaria], a more accurate alternative to PhB also tuned to nonprecessing simulations of BH-BH mergers; and (3) a nonspinning effective-one-body (EOB) model [@eob]. A detailed comparison of the three models can be found in [@Damour:2010zb]. Recent work by [@pannarale] shows that finite-size effects introduce negligible errors ($\lesssim 1\%$) in SNR calculations 