A template bank for gravitational waveforms from coalescing binary black holes: non-spinning binaries

Ajith, P.; Babak, S.; Chen, Y.; Hewitson, M.; Krishnan, B.; Sintes, A. M.; Whelan, J. T.; Bruegmann, B.; Diener, P.; Dorband, N.; Gonzalez, J.; Hannam, M.; Husa, S.; Pollney, D.; Rezzolla, L.; Santamaria, L.; Sperhake, U.; Thornburg, J.

doi:10.48550/arxiv.0710.2335

Cited by 50 publications

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“…This implies that the parameter space's dimensionality is effectively reduced from 6 to 2 (non-precessing) or 3 (precessing) [105][106][107] * * -at least for the inspiral waveforms. Based on experience with both the one-dimensional non-spinning case [80,86,88,90] and nonprecessing cases [87,91,92,109], we expect that in each parameter space's dimension ∼5 numerical-relativity waveforms will be sufficient. The feasibility of producing a nonprecessing-binary model using either a handful of non-precessing waveforms in the small mass ratio limit [109] and only two waveforms in the equal-mass case [85,87], or ∼5 2 = 25 waveforms in the comparable mass case, has been demonstrated in the EOB and phenomenological models in Refs.…”

Section: Spanning the Binary Parameter Spacementioning

confidence: 99%

“…A second class of phenomenological inspiral-merger-ringdown waveform models has also been developed, starting with [89,90]. In this case, the original motivation was to provide LIGO and Virgo detectors with inspiral, merger and ringdown waveforms that could be computed efficiently during searches and be used to observe high-mass binary black holes.…”

Section: Introductionmentioning

confidence: 99%

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Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration

Hinder,

Buonanno,

Boyle

et al. 2013

Preprint

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The Numerical-Relativity-Analytical-Relativity (NRAR) collaboration is a joint effort between members of the numerical relativity, analytical relativity and gravitational-wave data analysis communities. The goal of the NRAR collaboration is to produce numerical-relativity simulations of compact binaries and use them to develop accurate analytical templates for the LIGO/Virgo Collaboration to use in detecting gravitational-wave signals and extracting astrophysical information from them. We describe the results of the first stage of the NRAR project, which focused on producing an initial set of numerical waveforms from binary black holes with moderate mass ratios and spins, as well as one non-spinning binary configuration which has a mass ratio of 10. All of the numerical waveforms are analysed in a uniform and consistent manner, with numerical errors evaluated using an analysis code created by members of the NRAR collaboration. We compare previously-calibrated, non-precessing analytical waveforms, notably the effective-one-body (EOB) and phenomenological template families, to the newly-produced numerical waveforms. We find that when the binary's total mass is ∼ 100-200M , current EOB and phenomenological models of spinning, non-precessing binary waveforms have overlaps above 99% (for advanced LIGO) with all of the non-precessing-binary numerical waveforms with mass ratios ≤ 4, when maximizing over binary parameters. This implies that the loss of event rate due to modelling error is below 3%. Moreover, the non-spinning EOB waveforms previously calibrated to five non-spinning waveforms with mass ratio smaller than 6 have overlaps above 99.7% with the numerical waveform with a mass ratio of 10, without even maximizing on the binary parameters.

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Section: Spanning the Binary Parameter Spacementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration

Hinder,

Buonanno,

Boyle

et al. 2013

Preprint

View full text Add to dashboard Cite

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“…EOB models require solving for the time evolution of the binary inspiral to obtain the GW signal, which is computationally expensive and makes the dependence on parameters less transparent. More efficient waveform models are those that directly provide a description of the GWs in the frequency-domain, either from phenomenological models [31][32][33][34][35][36], reduced-order models for EOB [37][38][39][40], or surrogates of numerical-relativity (NR) waveforms [41,42]. Frequency-domain models calibrated to numerical-relativity (NR) simulations in the tidal sector [40,[43][44][45] phenomenologically describe an enhancement of matter effects compared to predictions from adiabatic tidal models, however, these models depend only on the tidal deformability parameters and are restricted in their parameter space coverage, hence are of limited applicability.…”

Section: Introductionmentioning

confidence: 99%

Frequency domain model of f -mode dynamic tides in gravitational waveforms from compact binary inspirals

Schmidt

Hinderer

2019

Phys. Rev. D

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The recent detection of gravitational waves (GWs) from the neutron star binary inspiral GW170817 has opened a unique avenue to probe matter and fundamental interactions in previously unexplored regimes. Extracting information on neutron star matter from the observed GWs requires robust and computationally efficient theoretical waveform models. We develop an approximate frequency-domain GW phase model of a main GW signature of matter: dynamic tides associated with the neutron stars' fundamental oscillation modes (f -modes). We focus on nonspinning objects on circular orbits and demonstrate that, despite its mathematical simplicity, the new "f -mode tidal" (fmtidal) model is in good agreement with the effective-one-body dynamical tides model up to GW frequencies of 1 kHz and gives physical meaning to part of the phenomenology captured in tidal models tuned to numerical-relativity. The advantages of the fmtidal model are that it makes explicit the dependence of the GW phasing on the characteristic equation-of-state parameters, i.e., tidal deformabilities and f -mode frequencies, is computationally efficient, and can readily be added to any frequency-domain baseline waveform. The fmtidal model is easily amenable to future improvements and provides the means for a first step towards independently measuring additional fundamental properties of neutron star matter beyond the tidal deformability as well as performing novel tests of General Relativity from GW observations. PACS numbers: 04.80.Nn, 95.85.Sz, 04.30.Tv, 97.60.Jd, 26.60.Kp * pschmidt@star.sr.bham.ac.uk † t.hinderer@uva.nl 1 Oscillation modes are characterized by three integers (n, , m),where n denotes the number of radial nodes in the mode function and m is the azimuthal integer. In the nonspinning case, the mode frequency is independent of m, and for the f -modes n = 0, hence our notation ω n m | f −mode = ω . arXiv:1905.00818v1 [gr-qc]

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“…We fix the integration constant C such that f PBH ≡ (ρ PBH /ρ DM ) zCMB is the PBH fraction at z = z CMB 1100. For the spectrum dE GW / dν we use commonly adopted fitting formulae [36][37][38][39].…”

Section: Gravitational Waves From Merging Black Holesmentioning

confidence: 99%

Towards closing the window of primordial black holes as dark matter: The case of large clustering

et al. 2019

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The idea of dark matter in the form of primordial black holes has seen a recent revival triggered by the LIGO detection of gravitational waves from binary black hole mergers. In this context, it has been argued that a large initial clustering of primordial black holes can help alleviate the strong constraints on this scenario. In this work, we show that on the contrary, with large initial clustering the problem is exacerbated and constraints on primordial black hole dark matter become overwhelmingly strong.

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A template bank for gravitational waveforms from coalescing binary black holes: non-spinning binaries

Cited by 50 publications

References 0 publications

Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration

Error-analysis and comparison to analytical models of numerical waveforms produced by the NRAR Collaboration

Frequency domain model of f -mode dynamic tides in gravitational waveforms from compact binary inspirals

Towards closing the window of primordial black holes as dark matter: The case of large clustering

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