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We estimate the expected signal-to-noise ratios (SNRs) from the three phases(inspiral,merger,ringdown) of coalescing binary black holes (BBHs) for initialand advanced ground-based interferometers (LIGO/VIRGO) and for space-basedinterferometers (LISA). LIGO/VIRGO can do moderate SNR (a few tens), moderateaccuracy studies of BBH coalescences in the mass range of a few to about 2000solar masses; LISA can do high SNR (of order 10^4) high accuracy studies in themass range of about 10^5 to 10^8 solar masses. BBHs might well be the firstsources detected by LIGO/VIRGO: they are visible to much larger distances (upto 500 Mpc by initial interferometers) than coalescing neutron star binaries(heretofore regarded as the "bread and butter" workhorse source for LIGO/VIRGO,visible to about 30 Mpc by initial interferometers). Low-mass BBHs (up to 50solar masses for initial LIGO interferometers; 100 for advanced; 10^6 for LISA)are best searched for via their well-understood inspiral waves; higher massBBHs must be searched for via their poorly understood merger waves and/or theirwell-understood ringdown waves. A matched filtering search for massive BBHsbased on ringdown waves should be capable of finding BBHs in the mass range ofabout 100 to 700 solar masses out to 200 Mpc (initial LIGO interferometers),and 200 to 3000 solar masses out to about z=1 (advanced interferometers). Therequired number of templates is of order 6000 or less. Searches based on mergerwaves could increase the number of detected massive BBHs by a factor of order10 or more over those found from inspiral and ringdown waves, without detailedknowledge of the waveform shapes, using a "noise monitoring" search algorithm.A full set of merger templates from numerical relativity could further increasethe number of detected BBHs by an additional factor of up to 4.Comment: 40 pages, Revtex, psfig.tex, seven figures, submitted to Phys Rev

Measuring gravitational waves from binary black hole coalescences. I. Signal to noise for inspiral, merger, and ringdown