Intensity and anisotropies of the stochastic gravitational wave background from merging compact binaries in galaxies

Capurri, Giulia; Lapi, A.; Baccigalupi, C.; Boco, Lumen; Ronconi, Tommaso

doi:10.1088/1475-7516/2021/11/032

Cited by 32 publications

(34 citation statements)

References 157 publications

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“…This framework is flexible and splits the cosmological large-scale structure and sub-galactic scales so that it can be applied to any source contributions and any frequency band. The astrophysical dependence of the angular power spectrum on the detail of the underlying astrophysical model has been studied in [25,[35][36][37][187][188][189][190] and different formal aspects of the derivation of anisotropies and their interpretation are discussed in [15,18,19,32,186]. The relative importance of cosmological and astrophysical effects depends on the frequency band chosen, hence offering the possibility to distinguish different astrophysical processes.…”

Section: Astrophysical Sources Of Anisotropiesmentioning

confidence: 99%

Probing Anisotropies of the Stochastic Gravitational Wave Background with LISA

Bartolo¹,

Bertacca²,

Caldwell³

et al. 2022

Preprint

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We investigate the sensitivity of the Laser Interferometer Space Antenna (LISA) to the anisotropies of the Stochastic Gravitational Wave Background (SGWB). We first discuss the main astrophysical and cosmological sources of SGWB which are characterized by anisotropies in the GW energy density, and we build a Signal-to-Noise estimator to quantify the sensitivity of LISA to different multipoles. We then perform a Fisher matrix analysis of the prospects of detectability of anisotropic features with LISA for individual multipoles, focusing on a SGWB with a power-law frequency profile. We compute the noise angular spectrum taking into account the specific scan strategy of the LISA detector. We analyze the case of the kinematic dipole and quadrupole generated by Doppler boosting an isotropic SGWB. We find that β Ω GW ∼ 2 × 10 −11 is required to observe a dipolar signal with LISA. The detector response to the quadrupole has a factor ∼ 10 3 β relative to that of the dipole. The characterization of the anisotropies, both from a theoretical perspective and from a map-making point of view, allows us to extract information that can be used to understand the origin of the SGWB, and to discriminate among distinct superimposed SGWB sources.

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Section: Astrophysical Sources Of Anisotropiesmentioning

confidence: 99%

Probing Anisotropies of the Stochastic Gravitational Wave Background with LISA

Bartolo¹,

Bertacca²,

Caldwell³

et al. 2022

Preprint

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“…Note that the propagation term includes contributions similar to those encountered in CMB anisotropy calculations: the Sachs-Wolfe effect, due to the local curvature at emission, and the integrated Sachs-Wolfe effect, due to the curvature perturbations encountered along the line-of-sight [106]; a Doppler term due to the source's peculiar velocity; and higher order effects such as gravitational lensing and redshift-space distortions [107]. All these terms have been the subject of intense study in recent years and both astrophysical and primordial contributions have been modelled extensively (see for example [108][109][110] for independent calculations of astrophysical background anisotropies and [50,103,111] for examples of primordial ones). The propagation term is often assumed to be negligible in the case of astrophysical backgrounds or it is directly included as part of the source term; in [112,113], it is expressly estimated and shown to account for at most ∼10% of the total anisotropy.…”

Section: Anisotropies In Stochastic Backgroundsmentioning

confidence: 99%

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Renzini¹,

Goncharov²,

Jenkins³

et al. 2022

Preprint

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The collection of individually resolvable gravitational wave (GW) events makes up a tiny fraction of all GW signals that reach our detectors, while most lie below the confusion limit and are undetected. Similarly to voices in a crowded room, the collection of unresolved signals gives rise to a background that is well-described via stochastic variables and, hence, referred to as the stochastic GW background (SGWB). In this review, we provide an overview of stochastic GW signals and characterise them based on features of interest such as generation processes and observational properties. We then review the current detection strategies for stochastic backgrounds, offering a ready-to-use manual for stochastic GW searches in real data. In the process, we distinguish between interferometric measurements of GWs, either by ground-based or space-based laser interferometers, and timing-residuals analyses with pulsar timing arrays (PTAs). These detection methods have been applied to real data both by large GW collaborations and smaller research groups, and the most recent and instructive results are reported here. We close this review with an outlook on future observations with third generation detectors, space-based interferometers, and potential noninterferometric detection methods proposed in the literature.

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“…The analysis carried out so far implicitly assumes that only the cosmological background contributes to the SGWB. However, in addition to this background, one also expects a background of gravitational waves arising from unresolved astrophysical sources to contribute to the SGWB and its anisotropies [64][65][66][67][68][69][70][71][72][73][74][75][76]. Detecting the cosmological background in the presence of this astrophysical foreground will be a major challenge and various methods to separate the monopoles of these backgrounds have been proposed in [77][78][79][80][81][82][83][84][85].…”

Section: Astrophysical Foregroundsmentioning

confidence: 99%

Testing the Early Universe with Anisotropies of the Gravitational Wave Background

Dimastrogiovanni,

Fasiello,

Malhotra

et al. 2021

Preprint

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In this work we analyse in detail the possibility of using small and intermediatescale gravitational wave anisotropies to constrain the inflationary particle content. First, we develop a phenomenological approach focusing on anisotropies generated by primordial tensor-tensor-scalar and purely gravitational non-Gaussianities. We highlight the quantities that play a key role in determining the detectability of the signal. To amplify the power of anisotropies as a probe of early universe physics, we consider cross-correlations with CMB temperature anisotropies. We assess the size of the signal from inflationary interactions against so-called induced anisotropies. In order to arrive at realistic estimates, we obtain the projected constraints on the non-linear primordial parameter F NL for several upcoming gravitational wave probes in the presence of the astrophysical gravitational wave background. We further illustrate our findings by considering a concrete inflationary realisation and use it to underscore a few subtleties in the phenomenological analysis.

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Intensity and anisotropies of the stochastic gravitational wave background from merging compact binaries in galaxies

Cited by 32 publications

References 157 publications

Probing Anisotropies of the Stochastic Gravitational Wave Background with LISA

Probing Anisotropies of the Stochastic Gravitational Wave Background with LISA

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Testing the Early Universe with Anisotropies of the Gravitational Wave Background

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