Observing gravitational waves from core-collapse supernovae in the advanced detector era

Gossan, S. E.; Sutton, P. J.; Stuver, A. L.; Zanolin, M.; Gill, K.; Ott, Christian D.

doi:10.1103/physrevd.93.042002

Cited by 124 publications

(126 citation statements)

References 172 publications

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“…We use the observational data taken by H1 and L1 during the S5 science run, and data taken by V1 during the VSR1 science run, which is now publicly available via the LIGO Open Science Center (LOSC) [82]. This data is recolored to the design sensitivity Power Spectral Density (PSD) of aLIGO and AdVirgo, as outlined in [14], which permits a more realistic estimation of the sensitivity of our analysis in future advanced detector observation runs. The detectors are expected to reach design sensitivity in 2019.…”

Section: Discussionmentioning

confidence: 99%

“…AdVirgo is a 3km Italian detector expected to join the aLIGO detector network early in 2017 [13]. Recent work by Gossan et al [14] shows that GWs from non-rotating and rotating core collapse may be observable throughout the Milky Way and the Large Magellanic Cloud (LMC). The rate for these sources is low at around 2 − 3 CCSNe per 100yr [15][16][17][18].…”

Section: Introductionmentioning

confidence: 99%

“…Firstly, signals were injected into data for one detector, assuming optimal orientation and sky location for maximal antenna sensitivity of the detector (see [14] for information on the antenna sensitivity of an interferometric GW detector). Given this, the time-varying antenna sensitivity for a given detector was not taken into account, and hence the antenna sensitivity considered was artificially optimistic.…”

Section: Introductionmentioning

confidence: 99%

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Inferring the core-collapse supernova explosion mechanism with gravitational waves

et al. 2016

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A detection of a core-collapse supernova (CCSN) gravitational-wave (GW) signal with an Advanced LIGO and Virgo detector network may allow us to measure astrophysical parameters of the dying massive star. GWs are emitted from deep inside the core and, as such, they are direct probes of the CCSN explosion mechanism. In this study we show how we can determine the CCSN explosion mechanism from a GW supernova detection using a combination of principal component analysis and Bayesian model selection. We use simulations of GW signals from CCSN exploding via neutrino-driven convection and rapidly-rotating core collapse. Previous studies have shown that the explosion mechanism can be determined using one LIGO detector and simulated Gaussian noise. As real GW detector noise is both non-stationary and non-Gaussian we use real detector noise from a network of detectors with a sensitivity altered to match the advanced detectors design sensitivity. For the first time we carry out a careful selection of the number of principal components to enhance our model selection capabilities. We show that with an advanced detector network we can determine if the CCSN explosion mechanism is neutrino-driven convection for sources in our Galaxy and rapidly-rotating core collapse for sources out to the Large Magellanic Cloud.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Inferring the core-collapse supernova explosion mechanism with gravitational waves

et al. 2016

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“…For each waveform, we give the emission type, journal reference, waveform identifier, angle-averaged root-sum-squared strain hrss, the frequency f peak at which the GW energy spectrum peaks, the emitted GW energy EGW, and available polarizations. See [73,142] Note that since the simulation producing this waveform was axisymmetric, only the + polarization is available.…”

Section: Waveforms From Multi-dimensional Ccsn Simulationsmentioning

confidence: 99%

“…Previous targeted GW searches have been carried out for gamma-ray bursts [62][63][64][65][66][67][68][69], softgamma repeater flares [70,71], and pulsar glitches [72]. A recent study [73] confirmed that targeted searches with Advanced LIGO and Virgo at design sensitivity should be able to detect neutrino-driven CCSNe out to several kiloparsecs and rapidly rotating CCSNe out to tens of kiloparsecs, while more extreme GW emission scenarios will be detectable to several megaparsecs. An extended analysis [74] of GW spectrograms show that several characteristic CCSN signal features can be extracted with KAGRA, Advanced LIGO and Virgo network.…”

Section: Introductionmentioning

confidence: 99%

First targeted search for gravitational-wave bursts from core-collapse supernovae in data of first-generation laser interferometer detectors

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. D

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We present results from a search for gravitational-wave bursts coincident with two core-collapse supernovae observed optically in 2007 and 2011. We employ data from the Laser Interferometer Gravitational-wave Observatory (LIGO), the Virgo gravitational-wave observatory, and the GEO 600 gravitational-wave observatory. The targeted core-collapse supernovae were selected on the basis of (1) proximity (within approximately 15 Mpc), (2) tightness of observational constraints on the time of core collapse that defines the gravitational-wave search window, and (3) coincident operation of 6 at least two interferometers at the time of core collapse. We find no plausible gravitational-wave candidates. We present the probability of detecting signals from both astrophysically well-motivated and more speculative gravitational-wave emission mechanisms as a function of distance from Earth, and discuss the implications for the detection of gravitational waves from core-collapse supernovae by the upgraded Advanced LIGO and Virgo detectors.

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Numerical Relativity and the Discovery of Gravitational Waves

Eisenstein¹

2019

Annalen der Physik

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Solving Einstein's equations precisely for strong-field gravitational systems is essential to determining the full physics content of gravitational wave detections. Without these solutions it is not possible to infer precise values for initial and final-state system parameters. Obtaining these solutions requires extensive numerical simulations, as Einstein's equations governing these systems are much too difficult to solve analytically. These difficulties arise principally from the curved, non-linear nature of spacetime in general relativity. Developing the numerical capabilities needed to produce reliable, efficient calculations has required a Herculean 50-year effort involving hundreds of researchers using sophisticated physical insight, algorithm development, computational technique, and computers that are a billion times more capable than they were in 1964 when computations were first attempted. The purpose of this review is to give an accessible overview for non-experts of the major developments that have made such dramatic progress possible. R. A. EisensteinMIT LIGO NW22-272, Figure 1 is a comparison of the observed strains, within a 35-350 Hz passband, at the Hanford and Livingston LIGO sites after shifting and inverting the Hanford data to account for the difference in arrival time and the relative orientation of the detectors. The event was identified nearly in real time using detection techniques that made minimal assumptions [4] about the nature of the incoming wave. Subsequent analysis used matched-filter techniques [5] to establish the statistical significance of the observation. Detailed statistical analyses using Bayesian methods were used to estimate the parameters of the coalescing BH-BH system. [3] Long before coalescence occurs, the two orbiting BHs can be represented as point masses co-rotating in a Newtonian orbit of very large size. In Einstein's Universe, however, an "inspiral" is taking place due to energy lost to gravitational radiation.This "inspiral" is indicated on the left side of Figure 2. As it progresses, the orbit becomes circularized due to the energy loss. The spacetime is basically flat except near each BH. Even so, Newtonian physics cannot accurately describe what is happening. Instead, "Post-Newtonian" (PN) [6] and "Effective One-Body" (EOB) [7] methods must be employed. [8] As the BHs near each other (center, Figure 2), spacetime begins to warp and the BH horizons are distorted. The EOB approach provides a good description (better than one might expect) until the beginning of coalescence, when the spacetime becomes significantly curved and highly non-linear. In fact, the inspiraling waveform depends strongly on several aspects of the BH-BH interaction, for example, their masses, spins, orbit orientation, and eccentricity. This dependence plays a key role in the extraction of those parameters, but requires fits to numerical relativity simulations (Section 4.9) to reproduce the correct result as the binary system approaches merger. Recently, parameter estimation methods have d...

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Observing gravitational waves from core-collapse supernovae in the advanced detector era

Cited by 124 publications

References 172 publications

Inferring the core-collapse supernova explosion mechanism with gravitational waves

Inferring the core-collapse supernova explosion mechanism with gravitational waves

First targeted search for gravitational-wave bursts from core-collapse supernovae in data of first-generation laser interferometer detectors

Numerical Relativity and the Discovery of Gravitational Waves

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