Matching post-Newtonian and numerical relativity waveforms: Systematic errors and a new phenomenological model for nonprecessing black hole binaries

By L. Santamaría, Frank Ohme, P. Ajith, B. Brügmann, N. Dorband, M. Hannam, Sascha Husa, P. Mösta, D. Pollney, Christian Reisswig and 3 more. 2010

300 citations recorded by the source corpus.

We present a new phenomenological gravitational waveform model for the inspiral and coalescence of nonprecessing 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 nonprecessing 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.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/a63bb3ff3ba947f567d1f0ce0e93c09ac1061f0f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Geophysics

Citations in the corpus

Science with the space-based interferometer eLISA. III: probing the expansion of the universe using gravitational wave standard sirens (2016, result): “ne, in the conservative scenario) we further correct the results of this analysis by using results obtained with aligned (or anti-aligned) spin inspiral-merger-ringdown (IMR) \PhenomC" waveforms [66] and a set of dedicated precessing-spin IMR hybrid waveforms (cf. the Appendix of Paper I). This”
The origin of spin in binary black holes (2019, background): “This is explained by the fact that the leading spinorbit-coupling term in the post-Newtonian waveforms is dominated by this parameter (Santamaría et al. 2010).”
Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, methodology): “The SNR is computed using PhenomC waveforms (Santamaría et al., 2010), which are inclusive of the three phases of black hole coalescence (in jargon: inspiral, merger, and ring-down, as described in the text).”
GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs (2018, background): “The effective aligned spin is defined as a simple mass-weighted linear combination of the spins [23,24,121] projected onto the Newtonian angular momentum L̂N , which is normal to the orbital plane (L̂ 1⁄4 L̂N for aligned-spin binaries)”
Binary Black Hole Mergers in the First Advanced LIGO Observing Run (2016, unknown): “and the effective spin parameter [71–76]”
Notes on the integration of numerical relativity waveforms (2010, methodology): “, [21, 12]).”
COMPACT BINARY MERGER RATES: COMPARISON WITH LIGO/VIRGO UPPER LIMITS (2015, methodology): “Our standard waveformmodel IMRPhenomC from Santamaria et al. (2010) includes inspiral, merger, and ringdown, and is tuned to numerical relativity simulations of non-precessing BH-BH mergers with aligned spins.”