Frequency-domain gravitational waves from nonprecessing black-hole binaries. I. New numerical waveforms and anatomy of the signal

By Sascha Husa, Sebastian Khan, M. Hannam, M. Purrer, Frank Ohme, X. J. Forteza, A. Boh'e. 2015

449 citations recorded by the source corpus.

In this paper we discuss the anatomy of frequency-domain gravitational-wave signals from nonprecessing black-hole coalescences with the goal of constructing accurate phenomenological waveform models. We first present new numerical-relativity simulations for mass ratios up to 18, including spins. From a comparison of different post-Newtonian approximants with numerical-relativity data we select the uncalibrated SEOBNRv2 model as the most appropriate for the purpose of constructing hybrid post-Newtonian/numerical-relativity waveforms, and we discuss how we prepare time-domain and frequency-domain hybrid data sets. We then use our data together with results in the literature to calibrate simple explicit expressions for the final spin and radiated energy. Equipped with our prediction for the final state we then develop a simple and accurate merger-ringdown model based on modified Lorentzians in the gravitational-wave amplitude and phase, and we discuss a simple method to represent the low frequency signal augmenting the TaylorF2 post-Newtonian approximant with terms corresponding to higher orders in the post-Newtonian expansion. We finally discuss different options for modelling the small intermediate frequency regime between inspiral and merger ringdown. A complete phenomenological model based on the present work is presented in a companion paper [S. Khan et al., following paper, Phys. Rev. D 93 044007 (2016)].

Subfields: Astronomy and Astrophysics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/6b90dc869cafde512fbbfcfe74e247dd57060b98

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Citations in the corpus

THE FINAL SPIN FROM BINARY BLACK HOLES IN QUASI-CIRCULAR ORBITS (2016, methodology): “…the mean (µ) and root-mean-square (rms, σ) of the residuals from the NR data, as well as χ2red, for the three aforementioned sets of coefficients, and for the formulae of Barausse & Rezzolla (2009), Husa et al (2016) and Healy et al. (2014) (which use 4, 11 and 19 coefficients, respectively).”
The effect of pair-instability mass loss on black-hole mergers (2016, methodology): “For each merger we model the full inspiral-merger-ringdown waveform using the IMRPhenomD gravitational waveform templates (Khan et al. 2016; Husa et al. 2016).”
Tests of general relativity with the binary black hole signals from the LIGO-Virgo catalog GWTC-1 (2019, unknown): “model SEOBNRv4 ROM for reasons of computational efficiency), and the phenomenological waveform family IMRPhenomPv2 [19, 58, 59] that models the effects of precessing spins using two effective parameters by twisting up the underlying aligned-spin model.”
The effect of the metallicity-specific star formation history on double compact object mergers (2019, methodology): “To evaluate the SNR for a given DCO system, we compute the waveforms for the appropriate masses using a combination of IMRPhenomPv2 (Hannam et al. 2014; Husa et al. 2016; Khan et al. 2016) and SEOBNRv3 (Pan et al. 2014; Babak, Taracchini & Buonanno 2017).”
GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run (2021, methodology): “For GW190425, the only O3a event in this catalog classified as a BNS, we follow previous analyses [8,135], and report findings using the IMRPhenomP_NRTidal waveform model [65,66], which is based upon the BBH model IMRPhenomPv2 [153,162,163] with the addition of EOS dependent self-spin effects and co”