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We investigate the problem of detecting gravitational waves from binaries ofnonspinning black holes with masses m = 5--20 Msun, moving on quasicircularorbits, which are arguably the most promising sources for first-generationground-based detectors. We analyze and compare all the currently availablepost--Newtonian approximations for the relativistic two-body dynamics; forthese binaries, different approximations predict different waveforms. We thenconstruct examples of detection template families that embed all theapproximate models, and that could be used to detect the truegravitational-wave signal (but not to characterize accurately its physicalparameters). We estimate that the fitting factor for our detection families is>~0.95 (corresponding to an event-rate loss <~15%) and we estimate that thediscretization of the template family, for ~10^4 templates, increases the lossto <~20%.Comment: 58 pages, 38 EPS figures, final PRD version; small corrections to GW  flux terms as per Blanchet et al., PRD 71, 129902(E)-129904(E) (2005

Detection template families for gravitational waves from the final stages of binary–black-hole inspirals: Nonspinning case