Implementing a search for aligned-spin neutron star-black hole systems with advanced ground based gravitational wave detectors

Canton, T. Dal; Nitz, A.; Lundgren, A. P.; Nielsen, A. B.; Brown, D. A.; Dent, T.; Harry, G. M.; Krishnan, B.; Miller, A.; Wette, K.; Wiesner, K.; Willis, J. L.

doi:10.1103/physrevd.90.082004

Cited by 192 publications

(227 citation statements)

References 88 publications

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“…Two different, largely independent, analyses have been implemented to search for stellar-mass BBH signals in the data of O1: PyCBC [2][3][4] and GstLAL [5][6][7]. Both these analyses employ matched filtering [52][53][54][55][56][57][58][59][60] with waveforms given by models based on general relativity [8,9] to search for gravitational waves from binary neutron stars, BBHs, and neutron star-black hole binaries.…”

Section: Search Resultsmentioning

confidence: 99%

“…[2][3][4], and the configuration used to analyze the first 16 days of O1 data, containing GW150914, is described in Ref. [44].…”

Section: Pycbc Analysismentioning

confidence: 99%

“…Here, we report on results of the search for BBHs. 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].…”

Section: Introductionmentioning

confidence: 99%

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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: Search Resultsmentioning

confidence: 99%

“…[2][3][4], and the configuration used to analyze the first 16 days of O1 data, containing GW150914, is described in Ref. [44].…”

Section: Pycbc Analysismentioning

confidence: 99%

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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show abstract

“…All waveforms used in this paper were generated by the PyCBC software [29][30][31], which implements LALSUITE [32] containing the coded waveforms. As a first approximation, time-dependent SpinDominatedWf was implemented in LALSUITE with the above described approximation for κ 1 and α, but with radiation reaction included in the evolution of the parameters φ n , ψ and the orbital angular frequency ω.…”

Section: Methods and Waveformsmentioning

confidence: 99%

Investigating the Poor Match among Different Precessing Gravitational Waveforms

et al. 2018

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Abstract:The sixfold direct detection of gravitational waves opened the era of gravitational wave astronomy. All of these gravitational waves were emitted by black hole or neutron star binaries. The determination of the parameters characterizing compact binaries requires the accurate knowledge of waveforms. Three different waveforms (Spin Dominated, SpinTaylorT4 and Spinning Effective One Body fitted to Numerical Relativity, SEOBNR) are considered in the spin-aligned and precessing cases, in the parameter ranges where the larger spin dominates over the orbital angular momentum. The degeneracy in the parameter space of each waveform is analyzed, then the matches among the waveforms are investigated. Our results show that in the spin-aligned case only the inspiral Spin-dominated and SpinTaylorT4 waveforms agree well with each other. The highest matches of these with SEOBNR are at different parameters as compared to where SEOBNR shows the best match with itself, reflecting SEOBNR being full inspiral-merger-ringdown waveform, with coefficients fitted to numerical relativity, rather than arising from post-Newtonian (PN) calculations. In the precessing case, the matches between the pairs of all waveforms are significantly lower. We identify possible causes of this in (1) the implementation of the angular dynamics carried out at different levels of accuracy for different waveforms; (2) differences in the inclusiveness of the merger process and in the PN coefficients of the inspiral waveforms (Spin-Dominated, SpinTaylorT4) and the full SEOBNR waveform.

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“…First, in the online searches, GW170104 was identified by inspection of low-latency triggers in L1 due to the temporary incorrect condition of the Hanford detector in the low-latency system [4,26]. The online low-latency search can provide alerts when a GW signal is propagated to the detectors within…”

mentioning

confidence: 99%

The first confirmed gravitational wave detection in LIGO’s second observational run

Jin

Fan

2017

Sci. China Phys. Mech. Astron.

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Citation: J. Li, and X. L. Fan, The first confirmed gravitational wave detection in LIGO's second observational run, Sci. China-Phys. Mech. Astron. 60, 120431 (2017), https://doi.org/10.1007/s11433-017- In this article, we describe the results concerning the third coincident signal GW170104 from the coalescence of binary black holes (BBHs) during the second observation run (O2). The result was obtained from the LIGO Scientific Collaboration and the Virgo Collaboration. Following the first and second gravitational waves (GWs) detections in the first observation run (O1) [1], recently LIGO has observed a third coincident signal GW170104 from the coalescence of BBHs during the second observation run (O2) [2]. The observation was made on January 4, 2017 at 10:11:58.6 UTC through the Hanford and Livingston detectors. The search procedures for this detection were similar to the previous events. With improved data quality and detector sensitivity, the LIGO and Virgo Collaborations found no evidence of instrumental or environmental noise that may have contributed to the GW170104 signal. Based on the matched filter method, the event was detected by the waveform-based PyCBC pipeline [3,4] with a network signal-to-noise ratio (SNR) of 13 and a false alarm rate of less than 1 in 70000 years; the event was later independently identified by other pipelines.From a coherent Bayesian analysis of the data in both detectors [5,6], the values of the source parameters were recovered by the collaborations with 90% credible intervals. The coalescence of BBHs was located at a luminosity distance, D L , or about 3 billion light years, which is the farthest dis-*Corresponding author (email: fanxilong@outlook.com) tance recorded so far. Therefore the successful detection of such a weak signal at a greater distance has given more confidence. The total mass of the source is ∼ 50M ⊙ , which is in the mass gap of the GW151226 source (∼21M ⊙ ) and the GW150914 source(∼62M ⊙ ). In theory, the formation of such BBHs systems is suggested in a sub-solar metallicity environment [7]. As a subdominant parameter of the BBHs, their effective inspiral spin is inferred, which implies that black holes might spin in any direction [2]. This is the first time that the LIGO and Virgo Collaborations have obtained experimental evidence to show that the spins of BBHs may be antialigned (not excluding zero spins), but the probability seems very low. This research is meaningful in distinguishing the theoretical models for BBHs' formation.Combined with previous events, it provides more confidence for the result of the general relativity (GR) testing. From the modified dispersion test [8][9][10][11][12][13][14][15][16] and waveform parametrized test [17][18][19][20][21][22][23][24][25], additional tight constraints on the deviations from GR were obtained. Until now, no significant departure from GR has been found.Searches: As with the searches from the previous detections, the analysis search for the source of GW170104, which is also included online and offline se...

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Implementing a search for aligned-spin neutron star-black hole systems with advanced ground based gravitational wave detectors

Cited by 192 publications

References 88 publications

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Binary Black Hole Mergers in the First Advanced LIGO Observing Run

Investigating the Poor Match among Different Precessing Gravitational Waveforms

The first confirmed gravitational wave detection in LIGO’s second observational run

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