Spectral properties of the post-merger gravitational-wave signal from binary neutron stars

Takami, Kentaro; Rezzolla, Luciano; Baiotti, Luca

doi:10.1103/physrevd.91.064001

Cited by 246 publications

(489 citation statements)

References 90 publications

(195 reference statements)

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“…Furthermore, this method could be adapted to constrain or search for other smallamplitude features that might be shared by a population of events, e.g. common parameterized post-Einsteinianlike [43] corrections to the inspiral phase of the mergers, or common equation-of-state-discriminating frequencies excited in hypermassive remnants of binary neutron star mergers [44][45][46][47][48][49][50][51][52][53][54]. In this latter example, one issue in adapting the coherent stacking method would be achieving phase alignment, due to the challenge in accurately calculating the details of the matter dynamics post-merger.…”

Section: Hypothesis Testingmentioning

confidence: 99%

Black Hole Spectroscopy with Coherent Mode Stacking

et al. 2017

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The measurement of multiple ringdown modes in gravitational waves from binary black hole mergers will allow for testing fundamental properties of black holes in General Relativity, and to constrain modified theories of gravity. To enhance the ability of Advanced LIGO/Virgo to perform such tasks, we propose a coherent mode stacking method to search for a chosen target mode within a collection of multiple merger events. We first rescale each signal so that the target mode in each of them has the same frequency, and then sum the waveforms constructively. A crucial element to realize this coherent superposition is to make use of a priori information extracted from the inspiral-merger phase of each event. To illustrate the method, we perform a study with simulated events targeting the = m = 3 ringdown mode of the remnant black holes. We show that this method can significantly boost the signal-to-noise ratio of the collective target mode compared to that of the single loudest event. Using current estimates of merger rates we show that it is likely that advanced-era detectors can measure this collective ringdown mode with one year of coincident data gathered at design sensitivity.Introduction. The recent detection of gravitational waves (GWs) emitted during the coalescence of binary black holes [1, 2] marked the beginning of the era of gravitational wave astronomy, a feat that heralds a boom of scientific discoveries to come. GWs not only provide a new window to our universe, they also offer a unique opportunity to test General Relativity (GR) in the dynamical and highly non-linear gravitational regime [3][4][5][6][7]. One celebrated prediction of GR is the uniqueness, or "no-hair" property of vacuum black holes (BHs) [8][9][10][11][12]: all isolated BHs are described by the Kerr family of solutions, each uniquely characterized by only its mass and spin [69]. This property has many wide-ranging consequences, the two most relevant here being (a) that the spacetime of an isolated binary black hole (BBH) inspiral is uniquely characterized by a small, finite set of parameters identifying the two BHs in the binary and the properties of the orbit, and (b) that this same set of parameters uniquely determines the merger remnant and the full spectrum of its quasinormal mode (QNM) ringdown waveform.This latter point forms the basis of black hole spectroscopy, where measurements of multiple ringdown modes are used to test this no-hair property. The idea is as follows. If the no-hair property holds, a measurement of the (complex) frequency of one QNM can be inverted to find a discrete set of possibilities for the spherical harmonic ( , m) plus overtone number n of the mode, and the BH mass M and spin parameter a = | S|/M 2 , where S is the BH spin angular momentum. However, if we have a priori information about the objects that merged to form the perturbed BH, then we also have information

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Section: Hypothesis Testingmentioning

confidence: 99%

Black Hole Spectroscopy with Coherent Mode Stacking

et al. 2017

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“…The approximation in Eq. (60) shows that δf peak =f peak depends only on Q and ρ. From Table I and comparing Figs.…”

Section: B Parameter Estimation For the Peak Frequencymentioning

confidence: 99%

“…(1), which depends on the peak frequency f peak , the quality factor Q, the 22 mode amplitude A 0 , the angle-dependent amplitude factor A r and phase offset ϕ 0 . We estimate the 22 mode frequency (f peak ) using the fit of [12] (see also [11,14,[58][59][60][61] for other fits)…”

Section: B MC Studymentioning

confidence: 99%

Gravitational wave spectroscopy of binary neutron star merger remnants with mode stacking

et al. 2018

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A binary neutron star coalescence event has recently been observed for the first time in gravitational waves, and many more detections are expected once current ground-based detectors begin operating at design sensitivity. As in the case of binary black holes, gravitational waves generated by binary neutron stars consist of inspiral, merger, and postmerger components. Detecting the latter is important because it encodes information about the nuclear equation of state in a regime that cannot be probed prior to merger. The postmerger signal, however, can only be expected to be measurable by current detectors for events closer than roughly ten megaparsecs, which given merger rate estimates implies a low probability of observation within the expected lifetime of these detectors. We carry out Monte Carlo simulations showing that the dominant postmerger signal (the l ¼ m ¼ 2 mode) from individual binary neutron star mergers may not have a good chance of observation even with the most sensitive future ground-based gravitational wave detectors proposed so far (the Einstein Telescope and Cosmic Explorer, for certain equations of state, assuming a full year of operation, the latest merger rates, and a detection threshold corresponding to a signal-to-noise ratio of 5). For this reason, we propose two methods that stack the postmerger signal from multiple binary neutron star observations to boost the postmerger detection probability. The first method follows a commonly used practice of multiplying the Bayes factors of individual events. The second method relies on an assumption that the mode phase can be determined from the inspiral waveform, so that coherent mode stacking of the data from different events becomes possible. We find that both methods significantly improve the chances of detecting the dominant postmerger signal, making a detection very likely after a year of observation with Cosmic Explorer for certain equations of state. We also show that in terms of detection, coherent stacking is more efficient in accumulating confidence for the presence of postmerger oscillations in a signal than the first method. Moreover, assuming the postmerger signal is detected with Cosmic Explorer via stacking, we estimate through a Fisher analysis that the peak frequency can be measured to a statistical error of ∼4-20 Hz for certain equations of state. Such an error corresponds to a neutron star radius measurement to within ∼15-56 m, a fractional relative error ∼4%, suggesting that systematic errors from theoretical modeling ð≳100 m) may dominate the error budget.

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“…Besides the prominent peak at f peak , there are several additional peaks in the spectra (see Fig.5). It is suggested that these minor peaks contains rich information of the NS structure [33,[67][68][69].…”

Section: Extraction Of Radius Information By Gw From Merger Remnant Nsmentioning

confidence: 99%

“…Recent numerical relativity simulations of the NS-NS mergers with finite-temperature EOS that can support NS with M ≈ 2M ⊙ [32][33][34] suggest that instead of collapsing to a BH, a massive NS is likely to be formed as the remnant of the merger of canonical mass binary, i.e, if the total binary mass is not extremely high as ≲ 2.8M ⊙ [35] (see also Refs. [36] for pioneering numerical relativity simulations with a simplified EOS).…”

Section: Overview Of Evolution Of Ns-ns and Gw From Itmentioning

confidence: 99%