Ready-to-use post-Newtonian gravitational waveforms for binary black holes with non-precessing spins: An update

TL;DR

This paper updates gravitational waveform models for non-precessing binary black holes by including higher-order spin effects in both phase and amplitude, enhancing template accuracy for gravitational wave detection.

Contribution

It provides new frequency domain phasing coefficients and amplitude corrections up to 3.5PN order for non-precessing spins, improving waveform models for gravitational wave analysis.

Findings

Updated phasing coefficients including quadratic and cubic spin terms

Added 2PN spin contributions to waveform amplitude

Enhanced templates for parameter estimation and detection

Abstract

For black-hole binaries whose spins are (anti-) aligned with respect to the orbital angular momentum of the binary, we compute the frequency domain phasing coefficients including the quadratic-in-spin terms up to the third post-Newtonian (3PN) order, the cubic-in-spin terms at the leading order, 3.5PN, and the spin-orbit effects up to the 4PN order. In addition, we obtain the 2PN spin contributions to the amplitude of the frequency-domain gravitational waveforms for non-precessing binaries, using recently derived expressions for the time-domain polarization amplitudes of binaries with generic spins, complete at that accuracy level. These two results are updates to Arun et al. (2009) [1] for amplitude and Wade et al. (2013) [2] for phasing. They should be useful to construct banks of templates that model accurately non-precessing inspiraling binaries, for parameter estimation studies, and or constructing analytical template families that accounts for the inspiral-merger-ringdown phases of the binary.