FINDCHIRP: An algorithm for detection of gravitational waves from inspiraling compact binaries

Allen, B.; Anderson, W. G.; Brady, P. R.; Brown, D. A.; Creighton, J. D. E.

doi:10.1103/physrevd.85.122006

Cited by 586 publications

(705 citation statements)

References 57 publications

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“…The matched-filter SNR ρ for each template waveform and each detector's data as a function of time is calculated according to [11,208] …”

Section: Appendix A: Search Descriptionmentioning

confidence: 99%

“…The search was performed using two independently implemented analyses, referred to as PyCBC [2][3][4] and GstLAL [5][6][7]. These analyses use a common set of template waveforms [8][9][10] but differ in their implementations of matched filtering [11,12], their use of detector data-quality information [13], the techniques used to mitigate the effect of non-Gaussian noise transients in the detector [5,14], and the methods for estimating the noise background of the search [3,15]. We obtain results that are consistent between the two analyses.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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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“…The matched-filter SNR ρ for each template waveform and each detector's data as a function of time is calculated according to [11,208] …”

Section: Appendix A: Search Descriptionmentioning

confidence: 99%

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

View full text Add to dashboard Cite

show abstract

“…In this approximation, only one complex-valued function is needed to characterize the gravitational wave signature from a binary: either the (l, m) = (2, 2) mode itself or the strain extracted along the binary angular momentum axis. This approach has been broadly adopted when comparing nonspinning numerical relativity simulations to one another [1] and to post-Newtonian [2][3][4][5] and other [6] approximations; when building hybrid waveforms that join systematic postNewtonian approximations to numerical relativity [7,8]; when constructing phenomenological approximations to numerical relativity waveforms [9][10][11]; and when searching for the gravitational wave signature of merging compact binaries with interferometric detectors [12]. For similar reasons, the gravitational wave signature from a nonprecessing unequal-mass binary can also be approximated by h +,× (t,Ĵ ), the radiation along the total angular momentum axisĴ.…”

Section: Introductionmentioning

confidence: 99%

IsJenough? Comparison of gravitational waves emitted along the total angular momentum direction with other preferred orientations

et al. 2012

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The gravitational wave signature emitted from a merging binary depends on the orientation of an observer relative to the binary. Previous studies suggest that emission along the total initial or total final angular momenta leads to both the strongest and simplest signal from a precessing compact binary. In this paper we describe a concrete counterexample: a binary with m1/m2 = 4, a1 = 0.6x = −a2, placed in orbit in the x, y plane. We extract the gravitational wave emission along several proposed emission directions, including the initial (Newtonian) orbital angular momentum; the final (≃ initial) total angular momentum; and the dominant principal axis of L (a L b) M . Using several diagnostics, we show that the suggested preferred directions are not representative. For example, only for a handful of other directions (p < ∼ 15%) will the gravitational wave signal have comparable shape to the one extracted along each of these fiducial directions, as measured by a generalized overlap (> 0.95). We conclude that the information available in just one direction (or mode) does not adequately encode the complexity of orientation-dependent emission for even short signals from merging black hole binaries. Future investigations of precessing, unequal-mass binaries should carefully explore and model their orientation-dependent emission.

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“…Searches for the inspiral GW signal from coalescing binaries are typically carried out using a matched-filtering technique and potentially large template banks [51][52][53]. The size and composition of these template banks is defined by the details of the targeted sources.…”

Section: A Coherent Waveburstmentioning

confidence: 99%

Prospects for high frequency burst searches following binary neutron star coalescence with advanced gravitational wave detectors

et al. 2014

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The equation of state plays a critical role in the physics of the merger of two neutron stars. Recent numerical simulations with microphysical equation of state suggest the outcome of such events depends on the mass of the neutron stars. For less massive systems, simulations favor the formation of a hypermassive, quasi-stable neutron star, whose oscillations produce a short, high frequency burst of gravitational radiation. Its dominant frequency content is tightly correlated with the radius of the neutron star, and its measurement can be used to constrain the supranuclear equation of state. In contrast, the merger of higher mass systems results in prompt gravitational collapse to a black hole. We have developed an algorithm which combines waveform reconstruction from a morphologyindependent search for gravitational wave transients with Bayesian model selection, to discriminate between post-merger scenarios and accurately measure the dominant oscillation frequency. We demonstrate the efficacy of the method using a catalogue of simulated binary merger signals in data from LIGO and Virgo, and we discuss the prospects for this analysis in advanced ground-based gravitational wave detectors. From the waveforms considered in this work and assuming an optimally oriented source, we find that the post-merger neutron star signal may be detectable by this technique to ∼ 10-25 Mpc. We also find that we successfully discriminate between the post-merger scenarios with ∼ 95% accuracy and determine the dominant oscillation frequency of surviving post-merger neutron stars to within ∼ 10 Hz, averaged over all detected signals. This leads to an uncertainty in the estimated radius of a non-rotating 1.6 M⊙ reference neutron star of ∼ 100 m.

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FINDCHIRP: An algorithm for detection of gravitational waves from inspiraling compact binaries

Cited by 586 publications

References 57 publications

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

IsJenough? Comparison of gravitational waves emitted along the total angular momentum direction with other preferred orientations

Prospects for high frequency burst searches following binary neutron star coalescence with advanced gravitational wave detectors

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