Statistical properties of astrophysical gravitational-wave backgrounds

Meacher, D.; Thrane, E.; Regimbau, T.

doi:10.1103/physrevd.89.084063

Cited by 30 publications

(26 citation statements)

References 46 publications

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“…Another promising detection method that has been tested in the context of the ET Mock Data Challenge ) for the population of NSNS is to examine the residual of the null stream, which contains no GW signal and arises from the sum of the three ET detectors. However, Meacher et al (2014) has shown that non-Gaussian backgrounds can be detected with no loss of sensitivity by the standard crosscorrelation statistic used for Gaussian backgrounds as long as there is a strong enough signal present in the observation time, even if they do not overlap. This results was verified by the standard cross-correlation used in the Einstein Telescope Mock Data Challenges .…”

Section: Resultsmentioning

confidence: 99%

Effect of metallicity on the gravitational-wave signal from the cosmological population of compact binary coalescences

Kowalska-Leszczynska

Regimbau

Bulik

et al. 2015

A&A

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Context. Recent studies on stellar evolution have shown that the properties of compact objects strongly depend on the metallicity of the environment in which they were formed. Aims. Using some very simple assumptions on the metallicity of the stellar populations, we explore how this property affects the unresolved gravitational-wave background from extragalactic compact binaries. Methods. We obtained a suit of models using population synthesis code, estimated the gravitational-wave background they produce, and discuss its detectability with second-(advanced LIGO, advanced Virgo) and third-(Einstein Telescope) generation detectors. Results. Our results show that the background is dominated by binary black holes for all considered models in the frequency range of terrestrial detectors, and that it could be detected in most cases by advanced LIGO/Virgo, and with Einstein Telescope with a very high signal-to-noise ratio. The observed peak in a gravitational-wave spectrum depends on the metallicity of the stellar population.

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Section: Resultsmentioning

confidence: 99%

Effect of metallicity on the gravitational-wave signal from the cosmological population of compact binary coalescences

Kowalska-Leszczynska

Regimbau

Bulik

et al. 2015

A&A

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“…These fluctuations are much smaller than the current local merger uncertainty [44]. The predictions may also be conservative.…”

mentioning

confidence: 84%

“…While Eq. (4) is derived by assuming a Gaussian background [6], it can also be applied to non-Gaussian backgrounds (with signals that are clearly separated in time) such as the binary black hole background considered here [44]. The different black curves shown in this plot illustrate the improvement in expected sensitivity in the coming years.…”

mentioning

confidence: 99%

GW150914: Implications for the Stochastic Gravitational-Wave Background from Binary Black Holes

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. Lett.

351

340

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The LIGO detection of the gravitational wave transient GW150914, from the inspiral and merger of two black holes with masses ≳30M ⊙ , suggests a population of binary black holes with relatively high mass. This observation implies that the stochastic gravitational-wave background from binary black holes, created from the incoherent superposition of all the merging binaries in the Universe, could be higher than previously expected. Using the properties of GW150914, we estimate the energy density of such a background from binary black holes. In the most sensitive part of the Advanced LIGO and Advanced Virgo band for stochastic backgrounds (near 25 Hz), we predict Ω GW ðf ¼ 25 HzÞ ¼ 1.1 þ2.7 −0.9 × 10 −9 with 90% confidence. This prediction is robustly demonstrated for a variety of formation scenarios with different parameters. The differences between models are small compared to the statistical uncertainty arising from the currently poorly constrained local coalescence rate. We conclude that this background is potentially measurable by the Advanced LIGO and Advanced Virgo detectors operating at their projected final sensitivity.

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“…Given the recent observations of binary black hole mergers GW150914 and GW151226 [6,7], we expect the SGWB to be nearly isotropic [8] and dominated [9] by compact binary coalescences [10][11][12]. The LIGO and Virgo Collaborations have pursued the search for an isotropic stochastic background from LIGO's first observational run [13].…”

Section: Directional Limits On Persistent Gravitational Waves From Admentioning

confidence: 99%

Directional Limits on Persistent Gravitational Waves from Advanced LIGO’s First Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. Lett.

108

131

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We employ gravitational-wave radiometry to map the gravitational waves stochastic background expected from a variety of contributing mechanisms and test the assumption of isotropy using data from Advanced LIGO's first observing run. We also search for persistent gravitational waves from point sources with only minimal assumptions over the 20 -1726 Hz frequency band. Finding no evidence of gravitational waves from either point sources or a stochastic background, we set limits at 90% confidence. For broadband point sources, we report upper limits on the gravitational wave energy flux per unit frequency in the range Fα,Θ(f ) < (0.1 − 56) × 10 −8 erg cm −2 s −1 Hz −1 (f /25 Hz) α−1 depending on the sky location Θ and the spectral power index α. For extended sources, we report upper limits on the fractional gravitational wave energy density required to close the Universe of Ω(f, Θ) < (0.39−7.6)×10−8 sr −1 (f /25 Hz) α depending on Θ and α. Directed searches for narrowband gravitational waves from astrophysically interesting objects (Scorpius X-1, Supernova 1987 A, and the Galactic Center) yield median frequency-dependent limits on strain amplitude of h0 < (6.7, 5.5, and 7.0) × 10 −25 respectively, at the most sensitive detector frequencies between 130 -175 Hz. This represents a mean improvement of a factor of 2 across the band compared to previous searches of this kind for these sky locations, considering the different quantities of strain constrained in each case.Introduction.-A stochastic gravitational-wave background (SGWB) is expected from a variety of mechanisms [1][2][3][4][5]. Given the recent observations of binary black hole mergers GW150914 and GW151226 [6,7], we expect the SGWB to be nearly isotropic [8] and dominated [9] by compact binary coalescences [10][11][12]. The LIGO and Virgo Collaborations have pursued the search for an isotropic stochastic background from LIGO's first observational run [13]. Here, we adopt an eyes-wide-open philosophy and relax the assumption of isotropy in order to allow for the greater range of possible signals. We search for an anisotropic background, which could indicate a richer, more interesting cosmology than current models. We present the results of a generalized search for a stochastic signal with an arbitrary angular distribution mapped over all directions in the sky.Our search has three components. First, we utilize a broadband radiometer analysis [14,15], optimized for detecting a small number of resolvable point sources. This method is not applicable to extended sources. Second, we employ a spherical harmonic decomposition [16,17], which can be employed for point sources but is better suited to extended sources. Last, we carry out a narrowband radiometer search directed at the sky position of three astrophysically interesting objects: Scorpius X-1 (Sco X-1) [18,19], Supernova 1987 [20,21], and the Galactic Center (GC) [22].These three search methods are capable of detecting a wide range of possible signals with only minimal assumptions about the signal morphology. ...

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Statistical properties of astrophysical gravitational-wave backgrounds

Cited by 30 publications

References 46 publications

Effect of metallicity on the gravitational-wave signal from the cosmological population of compact binary coalescences

Effect of metallicity on the gravitational-wave signal from the cosmological population of compact binary coalescences

GW150914: Implications for the Stochastic Gravitational-Wave Background from Binary Black Holes

Directional Limits on Persistent Gravitational Waves from Advanced LIGO’s First Observing Run

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