The Gravitational Wave Background from Coalescing Compact Binaries: A New Method

Evangelista, Edgard F. D.; Araújo, J. C. N. de

doi:10.1007/s13538-014-0272-0

Cited by 12 publications

(11 citation statements)

References 30 publications

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“…The nature of the AGWB may differ from its cosmological counterpart, expected to be stationary, unpolarized, statistically Gaussian and isotropic, by analogy with the cosmic microwave background. Many different sources may contribute to the AGWB, including black holes and neutron star mergers [35][36][37][38][39][40][41], supermassive black holes [42], exploding supernovae (SNe) [43], neutron stars [44][45][46], and stellar core collapse [47], population III binaries [48].…”

Section: Introductionmentioning

confidence: 99%

Anisotropy of the astrophysical gravitational wave background: Analytic expression of the angular power spectrum and correlation with cosmological observations

2017

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Unresolved sources of gravitational waves are at the origin of a stochastic gravitational wave background. While the computation of its mean density as a function of frequency in a homogeneous and isotropic universe is standard lore, the computation of its anisotropies requires to understand the coarse graining from local systems, to galactic scales and then to cosmology. An expression of the gravitational wave energy density valid in any general spacetime is derived. It is then specialized to a perturbed Friedmann-Lemaître spacetime in order to determine the angular power spectrum of this stochastic background as well as its correlation with other cosmological probes, such as the galaxy number counts and weak lensing. Our result for the angular power spectrum also provides an expression for the variance of the gravitational wave background.

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Section: Introductionmentioning

confidence: 99%

Anisotropy of the astrophysical gravitational wave background: Analytic expression of the angular power spectrum and correlation with cosmological observations

2017

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“…This letter focuses on this last component of the AGWB to which many sources may contribute such as merging binary black holes (BH) and neutron stars (NS) [12][13][14][15][16][17], supermassive binary BH mergers [18][19][20][21][22], rotating NS [23][24][25], stellar core collapses [26,27]. Its properties depend on (1) local astrophysics through the energy spectrum of each kind of sources, (2) the host galaxies through the abundance of these systems and their evolution and (3) cosmology through the distribution of the large scale structure and history of merging of galaxies and clusters.…”

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confidence: 99%

First Predictions of the Angular Power Spectrum of the Astrophysical Gravitational Wave Background

et al. 2018

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We present the first predictions for the angular power spectrum of the astrophysical gravitational wave background constituted of the radiation emitted by all resolved and unresolved astrophysical sources. Its shape and amplitude depend on both the astrophysical properties on galactic scales and on cosmological properties. We show that the angular power spectrum behaves as C_{ℓ}∝1/ℓ on large scales and that relative fluctuations of the signal are of order 30% at 100 Hz. We also present the correlations of the astrophysical gravitational wave background with weak lensing and galaxy distribution. These numerical results pave the way to the study of a new observable at the crossroad between general relativity, astrophysics, and cosmology.

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“…26) and for stellar mass black holes and supermassive black holes, respectively n BH 10 −4 kpc −3 , (4.27) n SBH 10 −12 kpc −3 . PBH = βM with β < 10 3 this yields…”

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confidence: 99%

Polarization of a stochastic gravitational wave background through diffusion by massive structures

2019

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The geometric optics approximation traditionally used to study the propagation of gravitational waves on a curved background, breaks down in the vicinity of compact and extended astrophysical objects, where wave-like effects like diffusion and generation of polarization occur. We provide a framework to study the generation of polarization of a stochastic background of gravitational waves propagating in an inhomogeneous universe. The framework is general and can be applied to both cosmological and astrophysical gravitational wave backgrounds in any frequency range. We derive an order of magnitude estimate of the amount of polarization generated for cosmological and astrophysical backgrounds, in the frequency range covered by present and planned gravitational wave experiments. For an astrophysical background in the PTA and LISA band, the amount of polarization generated is suppressed by a factor 10 −4 (10 −5 ) with respect to anisotropies. For a cosmological background we get an additional 10 −2 suppression. We speculate on using our approach to map the distribution of (unresolvable) structures in the Universe.

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The Gravitational Wave Background from Coalescing Compact Binaries: A New Method

Cited by 12 publications

References 30 publications

Anisotropy of the astrophysical gravitational wave background: Analytic expression of the angular power spectrum and correlation with cosmological observations

Anisotropy of the astrophysical gravitational wave background: Analytic expression of the angular power spectrum and correlation with cosmological observations

First Predictions of the Angular Power Spectrum of the Astrophysical Gravitational Wave Background

Polarization of a stochastic gravitational wave background through diffusion by massive structures

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