Catalog of 174 Binary Black Hole Simulations for Gravitational Wave Astronomy

Mroué, Abdul; Scheel, Mark A.; Szilágyi, Béla; Pfeiffer, Harald P.; Boyle, Michael; Hemberger, Daniel A.; Kidder, Lawrence E.; Lovelace, Geoffrey; Ossokine, S.; Taylor, Nicholas W.; Zenginoğlu, Anıl; Buchman, Luisa T.; Chu, Tony; Foley, E.; Giesler, Matthew; Owen, Robert; Teukolsky, Saul A.

doi:10.1103/physrevlett.111.241104

Cited by 375 publications

(330 citation statements)

References 77 publications

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“…We provide a detailed evaluation of the source properties and inferred parameters of GW150914, GW151226, and LVT151012. We use models of the waveform covering the inspiral, merger, and ringdown phases based on combining post-Newtonian (PN) theory [19][20][21][22][23][24], the effective-onebody (EOB) formalism [25][26][27][28][29], and numerical relativity simulations [30][31][32][33][34][35][36]. One model is restricted to spins aligned with the orbital angular momentum [8,9], while the other allows for nonaligned orientation of the spins, which can lead to precession of the orbital plane [37,38].…”

Section: Introductionmentioning

confidence: 99%

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. X

1,234

1,383

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the first detections of gravitational waves from binary black hole mergers. In this paper, we present full results from a search for binary black hole merger signals with total masses up to 100M ⊙ and detailed implications from our observations of these systems. Our search, based on general-relativistic * Full author list given at the end of the article. † Deceased.Published by the American Physical Society under the terms of the Creative Commons Attribution 3.0 License. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI. BINARY BLACK HOLE MERGERS IN THE FIRST …PHYS. REV. X 6, 041015 (2016) 041015-5 models of gravitational-wave signals from binary black hole systems, unambiguously identified two signals, GW150914 and GW151226, with a significance of greater than 5σ over the observing period. It also identified a third possible signal, LVT151012, with substantially lower significance and with an 87% probability of being of astrophysical origin. We provide detailed estimates of the parameters of the observed systems. Both GW150914 and GW151226 provide an unprecedented opportunity to study the two-body motion of a compact-object binary in the large velocity, highly nonlinear regime. We do not observe any deviations from general relativity, and we place improved empirical bounds on several highorder post-Newtonian coefficients. From our observations, we infer stellar-mass binary black hole merger rates lying in the range 9-240 Gpc −3 yr −1 . These observations are beginning to inform astrophysical predictions of binary black hole formation rates and indicate that future observing runs of the Advanced detector network will yield many more gravitational-wave detections.

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Section: Introductionmentioning

confidence: 99%

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. X

1,234

1,383

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“…These PN approximants can differ from each other during the last hundreds of cycles before merger.] Yet NR simulations have been able to cover only tens of orbits [27][28][29] until now. This gap has emerged as one of the most important sources of uncertainty in present IMR waveform models.…”

mentioning

confidence: 99%

“…Halving the symmetric mass ratio ν (e.g., from m 1 =m 2 ¼ 2 to m 1 =m 2 ¼ 7) doubles T. Increasing the simulation length T is difficult: it becomes harder to preserve phase coherency, the outer boundary of a simulation is in causal contact for a larger fraction of the simulation, and existing codes would require many months or even years of wall-clock time. Therefore, progress toward longer simulations has been sluggish, with T increasing by only about a factor of 2 to 3 during the last five years [28,29,[31][32][33]. The duration T needed to close the gap depends on the binary parameters and the detector bandwidth.…”

mentioning

confidence: 99%

“…Both simulations are computed using the Spectral Einstein Code (SpEC) [35]. The short simulation uses established computational techniques [28]. The speed-up needed for the long simulation is the result of a series of code changes including task-based adaptive parallel load balancing, live timing-based selection of the most efficient algorithm (when multiple implementations of the same function are available), a modified memory layout to allow more efficient calls to low-level numerical packages, and a more efficient implementation of the generalized harmonic evolution equations.…”

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confidence: 99%

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Approaching the Post-Newtonian Regime with Numerical Relativity: A Compact-Object Binary Simulation Spanning 350 Gravitational-Wave Cycles

et al. 2015

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We present the first numerical-relativity simulation of a compact-object binary whose gravitational waveform is long enough to cover the entire frequency band of advanced gravitational-wave detectors, such as LIGO, Virgo, and KAGRA, for mass ratio 7 and total mass as low as 45.5M ⊙ . We find that effective-one-body models, either uncalibrated or calibrated against substantially shorter numericalrelativity waveforms at smaller mass ratios, reproduce our new waveform remarkably well, with a negligible loss in detection rate due to modeling error. In contrast, post-Newtonian inspiral waveforms and existing calibrated phenomenological inspiral-merger-ringdown waveforms display greater disagreement with our new simulation. The disagreement varies substantially depending on the specific post-Newtonian approximant used. [6]. The detection of GWs from compact-object binaries, as well as the determination of source properties from detected GW signals, relies on the accurate knowledge of the expected gravitational waveforms via matchedfiltering [7] and Bayesian methods [8].The need for accurate waveforms has motivated intense research. Early waveform models based on the postNewtonian (PN) formalism [9] were limited to the early inspiral. The effective-one-body (EOB) formalism [10,11] extended waveform models to the late inspiral, merger, and ringdown. Since 2005, research has greatly benefited from numerical-relativity (NR) simulations [12][13][14]. (Besides its importance for GW astronomy, NR has also deepened the understanding of general relativity in topics such as binary BH recoil [15,16], gravitational self-force [17], highenergy physics, and cosmology [18,19].) Current inspiral-merger-ringdown (IMR) waveform models [20][21][22][23]

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“…Second row shows gravitationalwave strain projected onto each detector in the 35-to 350-Hz band. Solid lines show a numerical relativity waveform (waveform shown is SXS:BBH:0305 available for download at www.black-holes.org/ waveforms) for a system with parameters consistent with those recovered from GW150914 (38,39) confirmed to 99.9% by an independent calculation based on ref. 40.…”

Section: Initial Ligo-the Era Of Upper Limitsmentioning

confidence: 87%

LIGO and the opening of a unique observational window on the universe

Kalogera

Lazzarini

2017

Proc. Natl. Acad. Sci. U.S.A.

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A unique window on the universe opened on September 14, 2015, with direct detection of gravitational waves by the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) detectors. This event culminated a half-century effort around the globe to develop terrestrial detectors of adequate sensitivity to achieve this goal. It also happened appropriately only a few months before the centennial of Einstein's final paper introducing the general theory of relativity. This detection provided the surprising discovery of a coalescing pair of "heavy" black holes (more massive than ≃25 M๏) leading to the formation of a spinning ≃62 solar mass black hole. One more binary black-hole detection and a significant candidate event demonstrated that a population of such merging binaries is formed in nature with a broad mass spectrum. This unique observational sample has already provided concrete measurements on the coalescence rates and has allowed us to test the theory of general relativity in the strong-field regime. As this nascent field of gravitational-wave astrophysics is emerging we are looking forward to the detection of binary mergers involving neutron stars and their electromagnetic counterparts, as well as continuous-wave sources, supernovae, a stochastic confusion background of compact-object mergers, known sources detected in unexpected ways, and completely unknown sources.

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Catalog of 174 Binary Black Hole Simulations for Gravitational Wave Astronomy

Cited by 375 publications

References 77 publications

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Approaching the Post-Newtonian Regime with Numerical Relativity: A Compact-Object Binary Simulation Spanning 350 Gravitational-Wave Cycles

LIGO and the opening of a unique observational window on the universe

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