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

TL;DR

This paper introduces a new phenomenological gravitational waveform model for non-precessing black hole binaries, combining post-Newtonian and numerical relativity data, and addresses systematic errors in waveform matching.

Contribution

It develops a frequency domain matching method and provides an analytical formula for the dominant gravitational wave mode, enhancing gravitational wave detection accuracy.

Findings

Dominant error source identified as post-Newtonian waveform inaccuracies near merger.

Analytical formula effectively captures hybrid waveform phenomenology.

Implementation improves gravitational wave search sensitivity.

Abstract

We present a new phenomenological gravitational waveform model for the inspiral and coalescence of non-precessing spinning black hole binaries. Our approach is based on a frequency domain matching of post-Newtonian inspiral waveforms with numerical relativity based binary black hole coalescence waveforms. We quantify the various possible sources of systematic errors that arise in matching post-Newtonian and numerical relativity waveforms, and we use a matching criteria based on minimizing these errors; we find that the dominant source of errors are those in the post-Newtonian waveforms near the merger. An analytical formula for the dominant mode of the gravitational radiation of non-precessing black hole binaries is presented that captures the phenomenology of the hybrid waveforms. Its implementation in the current searches for gravitational waves should allow cross-checks of other inspiral-merger-ringdown waveform families and improve the reach of gravitational wave searches.