Frequency-domain gravitational waves from nonprecessing black-hole binaries. II. A phenomenological model for the advanced detector era

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

646 citations recorded by the source corpus.

We present a new frequency-domain phenomenological model of the gravitational-wave signal from the inspiral, merger and ringdown of nonprecessing (aligned-spin) black-hole binaries. The model is calibrated to 19 hybrid effective-one-body–numerical-relativity waveforms up to mass ratios of 1∶18 and black-hole spins of |a/m|∼0.85 (0.98 for equal-mass systems). The inspiral part of the model consists of an extension of frequency-domain post-Newtonian expressions, using higher-order terms fit to the hybrids. The merger ringdown is based on a phenomenological ansatz that has been significantly improved over previous models. The model exhibits mismatches of typically less than 1% against all 19 calibration hybrids and an additional 29 verification hybrids, which provide strong evidence that, over the calibration region, the model is sufficiently accurate for all relevant gravitational-wave astronomy applications with the Advanced LIGO and Virgo detectors. Beyond the calibration region the model produces physically reasonable results, although we recommend caution in assuming that any merger-ringdown waveform model is accurate outside its calibration region. As an example, we note that an alternative nonprecessing model, SEOBNRv2 (calibrated up to spins of only 0.5 for unequal-mass systems), exhibits mismatch errors of up to 10% for high spins outside its calibration region. We conclude that waveform models would benefit most from a larger number of numerical-relativity simulations of high-aligned-spin unequal-mass binaries.

View Paper: https://www.semanticscholar.org/paper/0e05de9a898eb7573185ce785623ca5c8aed9e9f

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Citations in the corpus

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).”
Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA (2013, methodology): “Complementary rate estimation based upon astrophysical population models and observations of Galactic BNS systems (e.g., Abadie et al. 2010b; Kim et al. 2013; Dominik et al. 2015; Vangioni et al. 2016; de Mink and Belczynski 2015; Eldridge et al. 2017; Belczynski et al. 2017; Kruckow et al. 2018)…”
One Channel to Rule Them All? Constraining the Origins of Binary Black Holes Using Multiple Formation Pathways (2020, methodology): “We use the IMRPhenomPv2 waveform approximant (Hannam et al. 2014; Khan et al. 2016) for determining SNRs, and detector response functions are constructed using the PyCBC package (Nitz et al. 2019).”
Search for Gravitational Lensing Signatures in LIGO-Virgo Binary Black Hole Events (2019, methodology): “We then compute the optimal SNR ρ of signals observed by the Advanced LIGO-Virgo network using the IMRPHENOMPV2 waveform family (Hannam et al. 2014; Khan et al. 2016; Husa et al. 2016).”