Template-space metric for searches for gravitational waves from the inspiral, merger and ringdown of binary black holes

TL;DR

This paper derives a new template-space metric for IMR gravitational waveforms from binary black holes, improving template placement and search sensitivity in gravitational wave data analysis.

Contribution

It introduces a novel coordinate system and computes the IMR waveform metric, enhancing the accuracy of template bank construction for gravitational wave searches.

Findings

The metric agrees well with the exact match function.

It approximates other IMR waveform families effectively.

The metric can improve search sensitivity in advanced detectors.

Abstract

Searches for gravitational waves (GWs) from binary black holes using interferometric GW detectors require the construction of template banks for performing matched filtering while analyzing the data. Placement of templates over the parameter space of binaries, as well as coincidence tests of GW triggers from multiple detectors make use of the definition of a metric over the space of gravitational waveforms. Although recent searches have employed waveform templates coherently describing the inspiral, merger and ringdown (IMR) of the coalescence, the metric used in the template banks and coincidence tests was derived from post-Newtonian inspiral waveforms. In this paper, we compute the template-space metric of the IMR waveform family IMRPhenomB over the parameter space of masses and the effective spin parameter. We also propose a coordinate system, which is a modified version of post-Newtonian chirp time coordinates, in which the metric is slowly varying over the parameter space. The match function analytically computed using the metric has excellent agreement with the "exact" match function computed numerically. We show that the metric is able to provide a reasonable approximation to the match function of other IMR waveform families, such that the effective-one-body model calibrated to numerical relativity (EOBNRv2). The availability of this metric can contribute to improving the sensitivity of searches for GWs from binary black holes in the advanced detector era.