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We present a new phenomenological gravitational waveform model for theinspiral and coalescence of non-precessing spinning black hole binaries. Ourapproach is based on a frequency domain matching of post-Newtonian inspiralwaveforms with numerical relativity based binary black hole coalescencewaveforms. We quantify the various possible sources of systematic errors thatarise in matching post-Newtonian and numerical relativity waveforms, and we usea matching criteria based on minimizing these errors; we find that the dominantsource of errors are those in the post-Newtonian waveforms near the merger. Ananalytical formula for the dominant mode of the gravitational radiation ofnon-precessing black hole binaries is presented that captures the phenomenologyof the hybrid waveforms. Its implementation in the current searches forgravitational waves should allow cross-checks of other inspiral-merger-ringdownwaveform families and improve the reach of gravitational wave searches.

physical review. d. particles, fields, gravitation, and cosmology/physical review. d, particles, fields, gravitation, and cosmology

Matching post-Newtonian and numerical relativity waveforms: systematic  errors and a new phenomenological model for non-precessing black hole  binaries